TY  - JOUR
A1  - Abramowski, Attila
A1  - Acero, F.
A1  - Aharonian, Felix A.
A1  - Akhperjanian, A. G.
A1  - Anton, Gisela
A1  - Balenderan, Shangkari
A1  - Balzer, Arnim
A1  - Barnacka, Anna
A1  - Becherini, Yvonne
A1  - Tjus, J. Becker
A1  - Behera, B.
A1  - Bernlöhr, K.
A1  - Birsin, E.
A1  - Biteau, Jonathan
A1  - Bochow, A.
A1  - Boisson, Catherine
A1  - Bolmont, J.
A1  - Bordas, Pol
A1  - Brucker, J.
A1  - Brun, Francois
A1  - Brun, Pierre
A1  - Bulik, Tomasz
A1  - Carrigan, Svenja
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chadwick, Paula M.
A1  - Chaves, Ryan C. G.
A1  - Cheesebrough, A.
A1  - Colafrancesco, Sergio
A1  - Cologna, Gabriele
A1  - Conrad, Jan
A1  - Couturier, C.
A1  - Dalton, M.
A1  - Daniel, M. K.
A1  - Davids, I. D.
A1  - Degrange, B.
A1  - Deil, C.
A1  - deWilt, P.
A1  - Dickinson, H. J.
A1  - Djannati-Ataï, A.
A1  - Domainko, W.
A1  - Drury, L. O'C.
A1  - Dubus, G.
A1  - Dutson, K.
A1  - Dyks, J.
A1  - Dyrda, M.
A1  - Egberts, Kathrin
A1  - Eger, P.
A1  - Espigat, P.
A1  - Fallon, L.
A1  - Farnier, C.
A1  - Fegan, S.
A1  - Feinstein, F.
A1  - Fernandes, M. V.
A1  - Fernandez, D.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Foester, A.
A1  - Fuessling, M.
A1  - Gajdus, M.
A1  - Gallant, Y. A.
A1  - Garrigoux, T.
A1  - Gast, H.
A1  - Giebels, B.
A1  - Glicenstein, J. F.
A1  - Glueck, B.
A1  - Goeing, D.
A1  - Grondin, M. -H.
A1  - Grudzinska, M.
A1  - Haeffner, S.
A1  - Hague, J. D.
A1  - Hahn, J.
A1  - Hampf, D.
A1  - Harris, J.
A1  - Hauser, M.
A1  - Heinz, S.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hillert, A.
A1  - Hinton, James Anthony
A1  - Hofmann, W.
A1  - Hofverberg, P.
A1  - Holler, Markus
A1  - Horns, D.
A1  - Jacholkowska, A.
A1  - Jahn, C.
A1  - Jamrozy, M.
A1  - Jung, I.
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katz, U.
A1  - Kaufmann, S.
A1  - Khelifi, B.
A1  - Klepser, S.
A1  - Klochkov, D.
A1  - Kluzniak, W.
A1  - Kneiske, T.
A1  - Komin, Nu.
A1  - Kosack, K.
A1  - Kossakowski, R.
A1  - Krayzel, F.
A1  - Krueger, P. P.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lefaucheur, J.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J. -P.
A1  - Lennarz, D.
A1  - Lohse, T.
A1  - Lopatin, A.
A1  - Lu, C. -C.
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Masbou, J.
A1  - Maurin, G.
A1  - Maxted, N.
A1  - Mayer, M.
A1  - McComb, T. J. L.
A1  - Medina, M. C.
A1  - Mehault, J.
A1  - Menzler, U.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Moulin, Emmanuel
A1  - Naumann, C. L.
A1  - Naumann-Godo, M.
A1  - de Naurois, M.
A1  - Nedbal, D.
A1  - Nguyen, N.
A1  - Niemiec, J.
A1  - Nolan, S. J.
A1  - Ohm, S.
A1  - Wilhelmi, E. de Ona
A1  - Opitz, B.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Arribas, M. Paz
A1  - Pekeur, N. W.
A1  - Pelletier, G.
A1  - Perez, J.
A1  - Petrucci, P. -O.
A1  - Peyaud, B.
A1  - Pita, S.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Raue, M.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - de los Reyes, R.
A1  - Rieger, F.
A1  - Ripken, J.
A1  - Rob, L.
A1  - Rosier-Lees, S.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Sahakian, V.
A1  - Sanchez, David M.
A1  - Santangelo, Andrea
A1  - Schlickeiser, R.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwarzburg, S.
A1  - Schwemmer, S.
A1  - Sheidaei, F.
A1  - Skilton, J. L.
A1  - Sol, H.
A1  - Spengler, G.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Stinzing, F.
A1  - Stycz, K.
A1  - Sushch, Iurii
A1  - Szostek, A.
A1  - Tavernet, J. -P.
A1  - Terrier, R.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Valerius, K.
A1  - van Eldik, C.
A1  - Vasileiadis, G.
A1  - Venter, C.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Voelk, H. J.
A1  - Volpe, F.
A1  - Vorobiov, S.
A1  - Vorster, M.
A1  - Wagner, S. J.
A1  - Ward, M.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Wouters, D.
A1  - Zacharias, M.
A1  - Zajczyk, A.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zechlin, H. S.
T1  - HESS discovery of VHE gamma-rays from the quasar PKS 1510-089
JF  - Astronomy and astrophysics : an international weekly journal
N2  - The quasar PKS 1510-089 (z = 0.361) was observed with the H.E.S.S. array of imaging atmospheric Cherenkov telescopes during high states in the optical and GeV bands, to search for very high energy (VHE, defined as E >= 0.1 TeV) emission. VHE gamma-rays were detected with a statistical significance of 9.2 standard deviations in 15.8 h of H. E. S. S. data taken during March and April 2009. A VHE integral flux of I(0.15 TeV < E < 1.0TeV) = (1.0 +/- 0.2(stat) +/- 0.2(sys)) x 10(-11) cm(-2) s(-1) is measured. The best-fit power law to the VHE data has a photon index of G = 5.4 +/- 0.7(stat) +/- 0.3(sys). The GeV and optical light curves show pronounced variability during the period of H.E.S.S. observations. However, there is insufficient evidence to claim statistically significant variability in the VHE data. Because of its relatively high redshift, the VHE flux from PKS 1510-089 should suffer considerable attenuation in the intergalactic space due to the extragalactic background light (EBL). Hence, the measured gamma-ray spectrum is used to derive upper limits on the opacity due to EBL, which are found to be comparable with the previously derived limits from relatively-nearby BL Lac objects. Unlike typical VHE-detected blazars where the broadband spectrum is dominated by nonthermal radiation at all wavelengths, the quasar PKS 1510-089 has a bright thermal component in the optical to UV frequency band. Among all VHE detected blazars, PKS 1510-089 has the most luminous broad line region. The detection of VHE emission from this quasar indicates a low level of gamma - gamma absorption on the internal optical to UV photon field.
KW  - gamma rays: galaxies
KW  - quasars: individual: PKS 1510-089
KW  - infrared: diffuse background
Y1  - 2013
U6  - https://doi.org/10.1051/0004-6361/201321135
SN  - 0004-6361
VL  - 554
IS  - 6
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Abramowski, Attila
A1  - Acero, F.
A1  - Aharonian, Felix A.
A1  - Benkhali, Faical  Ait
A1  - Akhperjanian, A. G.
A1  - Angüner, Ekrem Oǧuzhan
A1  - Anton, Gisela
A1  - Balenderan, Shangkari
A1  - Balzer, Arnim
A1  - Barnacka, Anna
A1  - Becherini, Yvonne
A1  - Tjus, J. Becker
A1  - Bernlöhr, K.
A1  - Birsin, E.
A1  - Bissaldi, E.
A1  - Biteau, Jonathan
A1  - Boisson, Catherine
A1  - Bolmont, J.
A1  - Bordas, Pol
A1  - Brucker, J.
A1  - Brun, Francois
A1  - Brun, Pierre
A1  - Bulik, Tomasz
A1  - Carrigan, Svenja
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chadwick, Paula M.
A1  - Chalme-Calvet, R.
A1  - Chaves, Ryan C. G.
A1  - Cheesebrough, A.
A1  - Chretien, M.
A1  - Colafrancesco, Sergio
A1  - Cologna, Gabriele
A1  - Conrad, Jan
A1  - Couturier, C.
A1  - Dalton, M.
A1  - Daniel, M. K.
A1  - Davids, I. D.
A1  - Degrange, B.
A1  - Deil, C.
A1  - deWilt, P.
A1  - Dickinson, H. J.
A1  - Djannati-Ataï, A.
A1  - Domainko, W.
A1  - Drury, L. O'C.
A1  - Dubus, G.
A1  - Dutson, K.
A1  - Dyks, J.
A1  - Dyrda, M.
A1  - Edwards, T.
A1  - Egberts, Kathrin
A1  - Eger, P.
A1  - Espigat, P.
A1  - Farnier, C.
A1  - Fegan, S.
A1  - Feinstein, F.
A1  - Fernandes, M. V.
A1  - Fernandez, D.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Foerster, A.
A1  - Fuessling, M.
A1  - Gajdus, M.
A1  - Gallant, Y. A.
A1  - Garrigoux, T.
A1  - Gast, H.
A1  - Giebels, B.
A1  - Glicenstein, J. F.
A1  - Goering, D.
A1  - Grondin, M. -H.
A1  - Grudzinska, M.
A1  - Haeffner, S.
A1  - Hague, J. D.
A1  - Hahn, J.
A1  - Harris, J.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hervet, O.
A1  - Hillert, A.
A1  - Hinton, James Anthony
A1  - Hofmann, W.
A1  - Hofverberg, P.
A1  - Holler, Markus
A1  - Horns, D.
A1  - Jacholkowska, A.
A1  - Jahn, C.
A1  - Jamrozy, M.
A1  - Janiak, M.
A1  - Jankowsky, F.
A1  - Jung, I.
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katz, U.
A1  - Kaufmann, S.
A1  - Khelifi, B.
A1  - Kieffer, M.
A1  - Klepser, S.
A1  - Klochkov, D.
A1  - Kluzniak, W.
A1  - Kneiske, T.
A1  - Kolitzus, D.
A1  - Komin, Nu.
A1  - Kosack, K.
A1  - Krakau, S.
A1  - Krayzel, F.
A1  - Krueger, P. P.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lefaucheur, J.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J-P.
A1  - Lennarz, D.
A1  - Lohse, T.
A1  - Lopatin, A.
A1  - Lu, C-C.
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Marx, R.
A1  - Maurin, G.
A1  - Maxted, N.
A1  - Mayer, M.
A1  - McComb, T. J. L.
A1  - Medina, M. C.
A1  - Mehault, J.
A1  - Menzler, U.
A1  - Meyer, M.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Moulin, Emmanuel
A1  - Murach, T.
A1  - Naumann, C. L.
A1  - de Naurois, M.
A1  - Nedbal, D.
A1  - Niemiec, J.
A1  - Nolan, S. J.
A1  - Oakes, L.
A1  - Ohm, S.
A1  - Wilhelmi, E. de Ona
A1  - Opitz, B.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Arribas, M. Paz
A1  - Pekeur, N. W.
A1  - Pelletier, G.
A1  - Perez, J.
A1  - Petrucci, P-O.
A1  - Peyaud, B.
A1  - Pita, S.
A1  - Poon, H.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Raue, M.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - de los Reyes, R.
A1  - Rieger, F.
A1  - Rob, L.
A1  - Rosier-Lees, S.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Sahakian, V.
A1  - Sanchez, David M.
A1  - Santangelo, Andrea
A1  - Schlickeiser, R.
A1  - Schuessler, F.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwarzburg, S.
A1  - Schwemmer, S.
A1  - Sol, H.
A1  - Spengler, G.
A1  - Spiess, F.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Stinzing, F.
A1  - Stycz, K.
A1  - Sushch, Iurii
A1  - Szostek, A.
A1  - Tavernet, J-P.
A1  - Terrier, R.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Valerius, K.
A1  - van Eldik, C.
A1  - Vasileiadis, G.
A1  - Venter, C.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Voelk, H. J.
A1  - Volpe, F.
A1  - Vorster, M.
A1  - Wagner, S. J.
A1  - Wagner, P.
A1  - Ward, M.
A1  - Weidinger, M.
A1  - Weitzel, Q.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Willmann, P.
A1  - Woernlein, A.
A1  - Wouters, D.
A1  - Zacharias, M.
A1  - Zajczyk, A.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zechlin, H-S.
T1  - Constraints on axionlike particles with HESS from the irregularity of the PKS 2155-304 energy spectrum
JF  - Physical review : D, Particles, fields, gravitation, and cosmology
N2  - Axionlike particles (ALPs) are hypothetical light (sub-eV) bosons predicted in some extensions of the Standard Model of particle physics. In astrophysical environments comprising high-energy gamma rays and turbulent magnetic fields, the existence of ALPs can modify the energy spectrum of the gamma rays for a sufficiently large coupling between ALPs and photons. This modification would take the form of an irregular behavior of the energy spectrum in a limited energy range. Data from the H. E. S. S. observations of the distant BL Lac object PKS 2155 - 304 (z = 0.116) are used to derive upper limits at the 95% C. L. on the strength of the ALP coupling to photons, g(gamma a) < 2.1 x 10(-11) GeV-1 for an ALP mass between 15 and 60 neV. The results depend on assumptions on the magnetic field around the source, which are chosen conservatively. The derived constraints apply to both light pseudoscalar and scalar bosons that couple to the electromagnetic field.
Y1  - 2013
U6  - https://doi.org/10.1103/PhysRevD.88.102003
SN  - 1550-7998
SN  - 1550-2368
VL  - 88
IS  - 10
PB  - American Physical Society
CY  - College Park
ER  - 
TY  - JOUR
A1  - Abdalla, Hassan E.
A1  - Aharonian, Felix A.
A1  - Benkhali, F. Ait
A1  - Angüner, Ekrem Oǧuzhan
A1  - Arakawa, M.
A1  - Arcaro, C.
A1  - Armand, C.
A1  - Backes, M.
A1  - Barnard, M.
A1  - Becherini, Y.
A1  - Berge, D.
A1  - Bernloehr, K.
A1  - Blackwell, R.
A1  - Bottcher, M.
A1  - Boisson, C.
A1  - Bolmont, J.
A1  - Bonnefoy, S.
A1  - Bregeon, J.
A1  - Brun, F.
A1  - Brun, P.
A1  - Bryan, M.
A1  - Buechele, M.
A1  - Bulik, T.
A1  - Bylund, T.
A1  - Capasso, M.
A1  - Caroff, S.
A1  - Carosi, A.
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chakraborty, N.
A1  - Chand, T.
A1  - Chandra, S.
A1  - Chaves, R. C. G.
A1  - Chen, A.
A1  - Colafrancesco, S.
A1  - Condon, B.
A1  - Davids, I. D.
A1  - Deil, C.
A1  - Devin, J.
A1  - deWilt, P.
A1  - Dirson, L.
A1  - Djannati-Atai, A.
A1  - Dmytriiev, A.
A1  - Donath, A.
A1  - Doroshenko, V
A1  - Dyks, J.
A1  - Egberts, Kathrin
A1  - Emery, G.
A1  - Ernenwein, J-P
A1  - Eschbach, S.
A1  - Feijen, K.
A1  - Fegan, S.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Funk, S.
A1  - Fuessling, M.
A1  - Gabici, S.
A1  - Gallant, Y. A.
A1  - Gate, F.
A1  - Giavitto, G.
A1  - Glawion, D.
A1  - Glicenstein, J. F.
A1  - Gottschall, D.
A1  - Grondin, M-H
A1  - Hahn, J.
A1  - Haupt, M.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hinton, James Anthony
A1  - Hofmann, W.
A1  - Hoischen, Clemens
A1  - Holch, Tim Lukas
A1  - Holler, M.
A1  - Horns, D.
A1  - Huber, D.
A1  - Iwasaki, H.
A1  - Jacholkowska, A.
A1  - Jamrozy, M.
A1  - Jankowsky, D.
A1  - Jankowsky, F.
A1  - Jouvin, L.
A1  - Jung-Richardt, I
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katsuragawa, M.
A1  - Katz, U.
A1  - Khangulyan, D.
A1  - Khelifi, B.
A1  - King, J.
A1  - Klepser, S.
A1  - Kluzniak, W.
A1  - Komin, Nu
A1  - Kosack, K.
A1  - Kostunin, D.
A1  - Kraus, M.
A1  - Lamanna, G.
A1  - Lau, J.
A1  - Lemiere, A.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J-P
A1  - Leser, Eva
A1  - Lohse, T.
A1  - Lopez-Coto, R.
A1  - Lypova, I
A1  - Malyshev, D.
A1  - Marandon, V
A1  - Marcowith, Alexandre
A1  - Mariaud, C.
A1  - Marti-Devesa, G.
A1  - Marx, R.
A1  - Maurin, G.
A1  - Maxted, N.
A1  - Meintjes, P. J.
A1  - Mitchell, A. M. W.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Mohrmann, L.
A1  - Moore, C.
A1  - Moulin, Emmanuel
A1  - Murach, T.
A1  - Nakashima, S.
A1  - de Naurois, M.
A1  - Ndiyavala, H.
A1  - Niederwanger, F.
A1  - Niemiec, J.
A1  - Oakes, L.
A1  - Odaka, H.
A1  - Ohm, S.
A1  - Wilhelmi, E. de Ona
A1  - Ostrowski, M.
A1  - Oya, I
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Perennes, C.
A1  - Petrucci, P-O
A1  - Peyaud, B.
A1  - Piel, Q.
A1  - Pita, S.
A1  - Poireau, V
A1  - Noel, A. Priyana
A1  - Prokhorov, D. A.
A1  - Prokoph, H.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Rauth, R.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - Rieger, F.
A1  - Rinchiuso, L.
A1  - Romoli, C.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Ruiz-Velasco, E.
A1  - Sahakian, V
A1  - Saito, S.
A1  - Sanchez, David M.
A1  - Santangelo, Andrea
A1  - Sasaki, M.
A1  - Schlickeiser, R.
A1  - Schussler, F.
A1  - Schulz, A.
A1  - Schutte, H.
A1  - Schwanke, U.
A1  - Schwemmer, S.
A1  - Seglar-Arroyo, M.
A1  - Senniappan, M.
A1  - Seyffert, A. S.
A1  - Shafi, N.
A1  - Shilon, I
A1  - Shiningayamwe, K.
A1  - Simoni, R.
A1  - Sinha, A.
A1  - Sol, H.
A1  - Specovius, A.
A1  - Spir-Jacob, M.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Steppa, Constantin Beverly
A1  - Takahashi, T.
A1  - Tavernet, J-P
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tibaldo, Luigi
A1  - Tiziani, D.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Tsirou, M.
A1  - Tsuji, N.
A1  - Tuffs, R.
A1  - Uchiyama, Y.
A1  - van der Walt, D. J.
A1  - van Eldik, C.
A1  - van Rensburg, C.
A1  - van Soelen, B.
A1  - Vasileiadis, G.
A1  - Veh, J.
A1  - Venter, C.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voisin, F.
A1  - Voelk, H. J.
A1  - Vuillaume, T.
A1  - Wadiasingh, Z.
A1  - Wagner, S. J.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Yang, R.
A1  - Yoneda, H.
A1  - Zaborov, D.
A1  - Zacharias, M.
A1  - Zanin, R.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Ziegler, A.
A1  - Zorn, J.
A1  - Zywucka, N.
T1  - H.E.S.S. and Suzaku observations of the Vela X pulsar wind nebula
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. Pulsar wind nebulae (PWNe) represent the most prominent population of Galactic very-high-energy gamma-ray sources and are thought to be an efficient source of leptonic cosmic rays. Vela X is a nearby middle-aged PWN, which shows bright X-ray and TeV gamma-ray emission towards an elongated structure called the cocoon. Aims. Since TeV emission is likely inverse-Compton emission of electrons, predominantly from interactions with the cosmic microwave background, while X-ray emission is synchrotron radiation of the same electrons, we aim to derive the properties of the relativistic particles and of magnetic fields with minimal modelling. Methods. We used data from the Suzaku XIS to derive the spectra from three compact regions in Vela X covering distances from 0.3 to 4 pc from the pulsar along the cocoon. We obtained gamma-ray spectra of the same regions from H.E.S.S. observations and fitted a radiative model to the multi-wavelength spectra. Results. The TeV electron spectra and magnetic field strengths are consistent within the uncertainties for the three regions, with energy densities of the order 10(-12) erg cm(-3). The data indicate the presence of a cutoff in the electron spectrum at energies of similar to 100 TeV and a magnetic field strength of similar to 6 mu G. Constraints on the presence of turbulent magnetic fields are weak. Conclusions. The pressure of TeV electrons and magnetic fields in the cocoon is dynamically negligible, requiring the presence of another dominant pressure component to balance the pulsar wind at the termination shock. Sub-TeV electrons cannot completely account for the missing pressure, which may be provided either by relativistic ions or from mixing of the ejecta with the pulsar wind. The electron spectra are consistent with expectations from transport scenarios dominated either by advection via the reverse shock or by diffusion, but for the latter the role of radiative losses near the termination shock needs to be further investigated in the light of the measured cutoff energies. Constraints on turbulent magnetic fields and the shape of the electron cutoff can be improved by spectral measurements in the energy range greater than or similar to 10 keV.
KW  - stars: winds, outflows
KW  - gamma rays: stars
KW  - radiation mechanisms: non-thermal
KW  - acceleration of particles
KW  - pulsars: individual: PSR B0833-45
Y1  - 2019
U6  - https://doi.org/10.1051/0004-6361/201935458
SN  - 1432-0746
VL  - 627
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Abdalla, Hassan E.
A1  - Aharonian, Felix A.
A1  - Benkhali, F. Ait
A1  - Anguener, E. O.
A1  - Arakawa, M.
A1  - Arcaro, C.
A1  - Armand, C.
A1  - Ashkar, H.
A1  - Backes, M.
A1  - Martins, V. Barbosa
A1  - Barnard, M.
A1  - Becherini, Y.
A1  - Berge, D.
A1  - Bernloehr, K.
A1  - Blackwell, R.
A1  - Boettcher, M.
A1  - Boisson, C.
A1  - Bolmont, J.
A1  - Bonnefoy, S.
A1  - Bregeon, J.
A1  - Breuhaus, M.
A1  - Brun, F.
A1  - Brun, P.
A1  - Bryan, M.
A1  - Buechele, M.
A1  - Bulik, T.
A1  - Bylund, T.
A1  - Capasso, M.
A1  - Caroff, S.
A1  - Carosi, A.
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chakraborty, N.
A1  - Chand, T.
A1  - Chandra, S.
A1  - Chaves, R. C. G.
A1  - Chen, A.
A1  - Colafrancesco, S.
A1  - Curylo, M.
A1  - Davids, I. D.
A1  - Deil, C.
A1  - Devin, J.
A1  - de Wilt, P.
A1  - Dirson, L.
A1  - Djannati-Atai, A.
A1  - Dmytriiev, A.
A1  - Donath, A.
A1  - Doroshenko, V
A1  - Dyks, J.
A1  - Egberts, Kathrin
A1  - Emery, G.
A1  - Ernenwein, J-p
A1  - Eschbach, S.
A1  - Feijen, K.
A1  - Fegan, S.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Funk, S.
A1  - Fuessling, M.
A1  - Gabici, S.
A1  - Gallant, Y. A.
A1  - Gate, F.
A1  - Giavitto, G.
A1  - Glawion, D.
A1  - Glicenstein, J. F.
A1  - Gottschall, D.
A1  - Grondin, M-H
A1  - Hahn, J.
A1  - Haupt, M.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hinton, James Anthony
A1  - Hofmann, W.
A1  - Hoischen, Clemens
A1  - Holch, Tim Lukas
A1  - Holler, M.
A1  - Horns, D.
A1  - Huber, D.
A1  - Iwasaki, H.
A1  - Jamrozy, M.
A1  - Jankowsky, D.
A1  - Jankowsky, F.
A1  - Jung-Richardt, I
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katsuragawa, M.
A1  - Katz, U.
A1  - Khangulyan, D.
A1  - Khelifi, B.
A1  - King, J.
A1  - Klepser, S.
A1  - Kluzniak, W.
A1  - Komin, Nu
A1  - Kosack, K.
A1  - Kostunin, D.
A1  - Kraus, M.
A1  - Lamanna, G.
A1  - Lau, J.
A1  - Lemiere, A.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J-P
A1  - Leser, Eva
A1  - Levy, C.
A1  - Lohse, T.
A1  - Lopez-Coto, R.
A1  - Lypova, I
A1  - Mackey, J.
A1  - Majumdar, J.
A1  - Malyshev, D.
A1  - Marandon, V
A1  - Marcowith, Alexandre
A1  - Mares, A.
A1  - Mariaud, C.
A1  - Marti-Devesa, G.
A1  - Marx, R.
A1  - Maurin, G.
A1  - Meintjes, P. J.
A1  - Mitchell, A. M. W.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Mohrmann, L.
A1  - Muller, J.
A1  - Moore, C.
A1  - Moulin, Emmanuel
A1  - Murach, T.
A1  - Nakashima, S.
A1  - de Naurois, M.
A1  - Ndiyavala, H.
A1  - Niederwanger, F.
A1  - Niemiec, J.
A1  - Oakes, L.
A1  - Odaka, H.
A1  - Ohm, S.
A1  - Wilhelmi, E. de Ona
A1  - Ostrowski, M.
A1  - Oya, I
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Perennes, C.
A1  - Petrucci, P-O
A1  - Peyaud, B.
A1  - Piel, Q.
A1  - Pita, S.
A1  - Poireau, V
A1  - Noel, A. Priyana
A1  - Prokhorov, D. A.
A1  - Prokoph, H.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Rauth, R.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Remy, Q.
A1  - Renaud, M.
A1  - Rieger, F.
A1  - Rinchiuso, L.
A1  - Romoli, C.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Ruiz-Velasco, E.
A1  - Sahakian, V
A1  - Saito, S.
A1  - Sanchez, David M.
A1  - Santangelo, Andrea
A1  - Sasaki, M.
A1  - Schlickeiser, R.
A1  - Schussler, F.
A1  - Schulz, A.
A1  - Schutte, H.
A1  - Schwanke, U.
A1  - Schwemmer, S.
A1  - Seglar-Arroyo, M.
A1  - Senniappan, M.
A1  - Seyffert, A. S.
A1  - Shafi, N.
A1  - Shiningayamwe, K.
A1  - Simoni, R.
A1  - Sinha, A.
A1  - Sol, H.
A1  - Specovius, A.
A1  - Spir-Jacob, M.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Steppa, Constantin Beverly
A1  - Takahashi, T.
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tiziani, D.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Tsirou, M.
A1  - Tsuji, N.
A1  - Tuffs, R.
A1  - Uchiyama, Y.
A1  - van der Walt, D. J.
A1  - van Eldik, C.
A1  - van Rensburg, C.
A1  - van Soelen, B.
A1  - Vasileiadis, G.
A1  - Veh, J.
A1  - Venter, C.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voisin, F.
A1  - Voelk, H. J.
A1  - Vuillaume, T.
A1  - Wadiasingh, Z.
A1  - Wagner, S. J.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Yang, R.
A1  - Yoneda, H.
A1  - Zacharias, M.
A1  - Zanin, R.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Ziegler, A.
A1  - Zorn, J.
A1  - Zywucka, N.
A1  - Maxted, N.
T1  - Upper limits on very-high-energy gamma-ray emission from core-collapse supernovae observed with H.E.S.S.
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Young core-collapse supernovae with dense-wind progenitors may be able to accelerate cosmic-ray hadrons beyond the knee of the cosmic-ray spectrum, and this may result in measurable gamma-ray emission. We searched for gamma-ray emission from ten super- novae observed with the High Energy Stereoscopic System (H.E.S.S.) within a year of the supernova event. Nine supernovae were observed serendipitously in the H.E.S.S. data collected between December 2003 and December 2014, with exposure times ranging from 1.4 to 53 h. In addition we observed SN 2016adj as a target of opportunity in February 2016 for 13 h. No significant gamma-ray emission has been detected for any of the objects, and upper limits on the >1 TeV gamma-ray flux of the order of similar to 10(-13) cm(-)(2)s(-1) are established, corresponding to upper limits on the luminosities in the range similar to 2 x 10(39) to similar to 1 x 10(42) erg s(-1). These values are used to place model-dependent constraints on the mass-loss rates of the progenitor stars, implying upper limits between similar to 2 x 10(-5) and similar to 2 x 10(-3) M-circle dot yr(-1) under reasonable assumptions on the particle acceleration parameters.
KW  - gamma rays: general
KW  - supernovae: general
KW  - cosmic rays
Y1  - 2019
U6  - https://doi.org/10.1051/0004-6361/201935242
SN  - 1432-0746
VL  - 626
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Abdalla, Hassan E.
A1  - Aharonian, Felix A.
A1  - Benkhali, F. Ait
A1  - Angüner, Ekrem Oǧuzhan
A1  - Arakawa, M.
A1  - Arcaro, C.
A1  - Armand, C.
A1  - Arrieta, M.
A1  - Backes, M.
A1  - Barnard, M.
A1  - Becherini, Y.
A1  - Tjus, J. Becker
A1  - Berge, D.
A1  - Bernloehr, K.
A1  - Blackwell, R.
A1  - Bottcher, M.
A1  - Boisson, C.
A1  - Bolmont, J.
A1  - Bonnefoy, S.
A1  - Bordas, Pol
A1  - Bregeon, J.
A1  - Brun, F.
A1  - Brun, P.
A1  - Bryan, M.
A1  - Buchele, M.
A1  - Bulik, T.
A1  - Bylund, T.
A1  - Capasso, M.
A1  - Caroff, S.
A1  - Carosi, A.
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chakraborty, N.
A1  - Chand, T.
A1  - Chandra, S.
A1  - Chaves, R. C. G.
A1  - Chen, A.
A1  - Colafrancesco, S.
A1  - Condon, B.
A1  - Davids, I. D.
A1  - Deil, C.
A1  - Devin, J.
A1  - deWilt, P.
A1  - Dirson, L.
A1  - Djannati-Atai, A.
A1  - Dmytriiev, A.
A1  - Donath, A.
A1  - Doroshenko, V.
A1  - Dyks, J.
A1  - Egberts, Kathrin
A1  - Emery, G.
A1  - Ernenwein, J. -P.
A1  - Eschbach, S.
A1  - Fegan, S.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Funk, S.
A1  - Fuessling, M.
A1  - Gabici, S.
A1  - Gallant, Y. A.
A1  - Gate, F.
A1  - Giavitto, G.
A1  - Glawion, D.
A1  - Glicenstein, J. F.
A1  - Gottschall, D.
A1  - Grondin, M. -H.
A1  - Hahn, J.
A1  - Haupt, M.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hinton, James Anthony
A1  - Hofmann, W.
A1  - Hoischen, Clemens
A1  - Holch, Tim Lukas
A1  - Holler, M.
A1  - Horns, D.
A1  - Huber, D.
A1  - Iwasaki, H.
A1  - Jacholkowska, A.
A1  - Jamrozy, M.
A1  - Jankowsky, D.
A1  - Jankowsky, F.
A1  - Jouvin, L.
A1  - Jung-Richardt, I.
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katsuragawa, M.
A1  - Katz, U.
A1  - Khangulyan, D.
A1  - Khelifi, B.
A1  - King, J.
A1  - Klepser, S.
A1  - Kluzniak, W.
A1  - Komin, Nu.
A1  - Kosack, K.
A1  - Kraus, M.
A1  - Lamanna, G.
A1  - Lau, J.
A1  - Lefaucheur, J.
A1  - Lemiere, A.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J. -P.
A1  - Leser, Eva
A1  - Lohse, T.
A1  - Lopez-Coto, R.
A1  - Lorentz, M.
A1  - Lypova, I.
A1  - Malyshev, D.
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Mariaud, C.
A1  - Marti-Devesa, G.
A1  - Marx, R.
A1  - Maurin, G.
A1  - Meintjes, P. J.
A1  - Mitchell, A. M. W.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Mohrmann, L.
A1  - Moore, C.
A1  - Moulin, Emmanuel
A1  - Murach, T.
A1  - Nakashima, S.
A1  - de Naurois, M.
A1  - Ndiyavala, H.
A1  - Niederwanger, F.
A1  - Niemiec, J.
A1  - Oakes, L.
A1  - Odaka, H.
A1  - Ohm, S.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Perennes, C.
A1  - Petrucci, P. -O.
A1  - Peyaud, B.
A1  - Piel, Q.
A1  - Pita, S.
A1  - Poireau, V.
A1  - Noel, A. Priyana
A1  - Prokhorov, D. A.
A1  - Prokoph, H.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Rauth, R.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - Rieger, F.
A1  - Rinchiuso, L.
A1  - Romoli, C.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Ruiz-Velasco, E.
A1  - Sahakian, V.
A1  - Saito, S.
A1  - Sanchez, David M.
A1  - Santangelo, Andrea
A1  - Sasaki, M.
A1  - Schlickeiser, R.
A1  - Schussler, F.
A1  - Schulz, A.
A1  - Schutte, H.
A1  - Schwanke, U.
A1  - Schwemmer, S.
A1  - Seglar-Arroyo, M.
A1  - Senniappan, M.
A1  - Seyffert, A. S.
A1  - Shafi, N.
A1  - Shilon, I.
A1  - Shiningayamwe, K.
A1  - Simoni, R.
A1  - Sinha, A.
A1  - Sol, H.
A1  - Specovius, A.
A1  - Spir-Jacob, M.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Steppa, Constantin Beverly
A1  - Takahashi, T.
A1  - Tavernet, J. -P.
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tiziani, D.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Tsirou, M.
A1  - Tsuji, N.
A1  - Tuffs, R.
A1  - Uchiyama, Y.
A1  - van der Walt, D. J.
A1  - van Eldik, C.
A1  - van Rensburg, C.
A1  - van Soelen, B.
A1  - Vasileiadis, G.
A1  - Veh, J.
A1  - Venter, C.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voisin, F.
A1  - Voelk, H. J.
A1  - Vuillaume, T.
A1  - Wadiasingh, Z.
A1  - Wagner, S. J.
A1  - Wagner, R. M.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Yang, R.
A1  - Yoneda, H.
A1  - Zaborov, D.
A1  - Zacharias, M.
A1  - Zanin, R.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Ziegler, A.
A1  - Zorn, J.
A1  - Zywucka, N.
T1  - H.E.S.S. observations of the flaring gravitationally lensed galaxy PKS 1830-211
JF  - Monthly notices of the Royal Astronomical Society
N2  - PKS 1830-211 is a known macrolensed quasar located at a redshift of z = 2.5. Its highenergy gamma-ray emission has been detected with the Fermi-Large Area Telescope (LAT) instrument and evidence for lensing was obtained by several authors from its high-energy data. Observations of PKS 1830-211 were taken with the High Energy Stereoscopic System (H.E.S.S.) array of Imaging Atmospheric Cherenkov Telescopes in 2014 August, following a flare alert by the Fermi-LAT Collaboration. The H.E.S.S observations were aimed at detecting a gamma-ray flare delayed by 20-27 d from the alert flare, as expected from observations at other wavelengths. More than 12 h of good-quality data were taken with an analysis threshold of similar to 67 GeV. The significance of a potential signal is computed as a function of the date and the average significance over the whole period. Data are compared to simultaneous observations by Fermi-LAT. No photon excess or significant signal is detected. An upper limit on PKS 1830-211 flux above 67 GeV is computed and compared to the extrapolation of the Fermi-LAT flare spectrum.
KW  - gravitational lensing: strong
KW  - diffuse radiation
KW  - gamma-rays: galaxies
Y1  - 2019
U6  - https://doi.org/10.1093/mnras/stz1031
SN  - 0035-8711
SN  - 1365-2966
VL  - 486
IS  - 3
SP  - 3886
EP  - 3891
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Abramowski, Attila
A1  - Aharonian, Felix A.
A1  - Benkhali, Faical  Ait
A1  - Akhperjanian, A. G.
A1  - Angüner, Ekrem Oǧuzhan
A1  - Backes, Michael
A1  - Balzer, Arnim
A1  - Becherini, Yvonne
A1  - Tjus, J. Becker
A1  - Berge, David
A1  - Bernhard, Sabrina
A1  - Bernlöhr, K.
A1  - Birsin, E.
A1  - Blackwell, R.
A1  - Boettcher, Markus
A1  - Boisson, Catherine
A1  - Bolmont, J.
A1  - Bordas, Pol
A1  - Bregeon, Johan
A1  - Brun, Francois
A1  - Brun, Pierre
A1  - Bryan, Mark
A1  - Bulik, Tomasz
A1  - Carr, John
A1  - Casanova, Sabrina
A1  - Chakraborty, N.
A1  - Chalme-Calvet, R.
A1  - Chaves, Ryan C. G.
A1  - Chen, Andrew
A1  - Chretien, M.
A1  - Colafrancesco, Sergio
A1  - Cologna, Gabriele
A1  - Conrad, Jan
A1  - Couturier, C.
A1  - Cui, Y.
A1  - Davids, I. D.
A1  - Degrange, B.
A1  - Deil, C.
A1  - deWilt, P.
A1  - Djannati-Ata, A.
A1  - Domainko, W.
A1  - Donath, A.
A1  - Dubus, G.
A1  - Dutson, K.
A1  - Dyks, J.
A1  - Dyrda, M.
A1  - Edwards, T.
A1  - Egberts, Kathrin
A1  - Eger, P.
A1  - Ernenwein, J-P.
A1  - Espigat, P.
A1  - Farnier, C.
A1  - Fegan, S.
A1  - Feinstein, F.
A1  - Fernandes, M. V.
A1  - Fernandez, D.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Foerster, A.
A1  - Fuessling, M.
A1  - Gabici, S.
A1  - Gajdus, M.
A1  - Gallant, Y. A.
A1  - Garrigoux, T.
A1  - Giavitto, G.
A1  - Giebels, B.
A1  - Glicenstein, J. F.
A1  - Gottschall, D.
A1  - Goyal, A.
A1  - Grondin, M-H.
A1  - Grudzinska, M.
A1  - Hadasch, D.
A1  - Haeffner, S.
A1  - Hahn, J.
A1  - Hawkes, J.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hervet, O.
A1  - Hillert, A.
A1  - Hinton, James Anthony
A1  - Hofmann, W.
A1  - Hofverberg, P.
A1  - Hoischen, Clemens
A1  - Holler, M.
A1  - Horns, D.
A1  - Ivascenko, A.
A1  - Jacholkowska, A.
A1  - Jamrozy, M.
A1  - Janiak, M.
A1  - Jankowsky, F.
A1  - Jung-Richardt, I.
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katz, U.
A1  - Kerszberg, D.
A1  - Khelifi, B.
A1  - Kieffer, M.
A1  - Klepser, S.
A1  - Klochkov, D.
A1  - Kluzniak, W.
A1  - Kolitzus, D.
A1  - Komin, Nu.
A1  - Kosack, K.
A1  - Krakau, S.
A1  - Krayzel, F.
A1  - Krueger, P. P.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lau, J.
A1  - Lefaucheur, J.
A1  - Lefranc, V.
A1  - Lemiere, A.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J-P.
A1  - Lohse, T.
A1  - Lopatin, A.
A1  - Lu, C-C.
A1  - Lui, R.
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Mariaud, C.
A1  - Marx, R.
A1  - Maurin, G.
A1  - Maxted, N.
A1  - Mayer, M.
A1  - Meintjes, P. J.
A1  - Menzler, U.
A1  - Meyer, M.
A1  - Mitchell, A. M. W.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Mora, K.
A1  - Moulin, Emmanuel
A1  - Murach, T.
A1  - de Naurois, M.
A1  - Niemiec, J.
A1  - Oakes, L.
A1  - Odaka, H.
A1  - Oettl, S.
A1  - Ohm, S.
A1  - Opitz, B.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Arribas, M. Paz
A1  - Pekeur, N. W.
A1  - Pelletier, G.
A1  - Petrucci, P-O.
A1  - Peyaud, B.
A1  - Pita, S.
A1  - Poon, H.
A1  - Prokoph, H.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Reichardt, I.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - de los Reyes, R.
A1  - Rieger, F.
A1  - Romoli, C.
A1  - Rosier-Lees, S.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Sahakian, V.
A1  - Salek, D.
A1  - Sanchez, David M.
A1  - Santangelo, Andrea
A1  - Sasaki, M.
A1  - Schlickeiser, R.
A1  - Schuessler, F.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwemmer, S.
A1  - Seyffert, A. S.
A1  - Simoni, R.
A1  - Sol, H.
A1  - Spanier, F.
A1  - Spengler, G.
A1  - Spies, F.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Stinzing, F.
A1  - Stycz, K.
A1  - Sushch, Iurii
A1  - Tavernet, J-P.
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Tuffs, R.
A1  - Valerius, K.
A1  - van der Walt, J.
A1  - van Eldik, C.
A1  - van Soelen, B.
A1  - Vasileiadis, G.
A1  - Veh, J.
A1  - Venter, C.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voisin, F.
A1  - Voelk, H. J.
A1  - Vuillaume, T.
A1  - Wagner, S. J.
A1  - Wagner, P.
A1  - Wagner, R. M.
A1  - Weidinger, M.
A1  - Weitzel, Q.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Willmann, P.
A1  - Woernlein, A.
A1  - Wouters, D.
A1  - Yang, R.
A1  - Zabalza, V.
A1  - Zaborov, D.
A1  - Zacharias, M.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zefi, F.
A1  - Zywucka, N.
T1  - Acceleration of petaelectronvolt protons in the Galactic Centre
JF  - Nature : the international weekly journal of science
N2  - Galactic cosmic rays reach energies of at least a few petaelectronvolts (of the order of 1015 electronvolts). This implies that our Galaxy contains petaelectronvolt accelerators (‘PeVatrons’), but all proposed models of Galactic cosmic-ray accelerators encounter difficulties at exactly these energies. Dozens of Galactic accelerators capable of accelerating particles to energies of tens of teraelectronvolts (of the order of 1013 electronvolts) were inferred from recent &#947;-ray observations3. However, none of the currently known accelerators—not even the handful of shell-type supernova remnants commonly believed to supply most Galactic cosmic rays—has shown the characteristic tracers of petaelectronvolt particles, namely, power-law spectra of &#947;-rays extending without a cut-off or a spectral break to tens of teraelectronvolts4. Here we report deep &#947;-ray observations with arcminute angular resolution of the region surrounding the Galactic Centre, which show the expected tracer of the presence of petaelectronvolt protons within the central 10 parsecs of the Galaxy. We propose that the supermassive black hole Sagittarius A* is linked to this PeVatron. Sagittarius A* went through active phases in the past, as demonstrated by X-ray outbursts5and an outflow from the Galactic Centre6. Although its current rate of particle acceleration is not sufficient to provide a substantial contribution to Galactic cosmic rays, Sagittarius A* could have plausibly been more active over the last 106–107 years, and therefore should be considered as a viable alternative to supernova remnants as a source of petaelectronvolt Galactic cosmic rays.
Y1  - 2016
U6  - https://doi.org/10.1038/nature17147
SN  - 0028-0836
SN  - 1476-4687
VL  - 531
SP  - 476
EP  - +
PB  - Nature Publ. Group
CY  - London
ER  - 
TY  - GEN
A1  - Abramowski, Attila
A1  - Aharonian, Felix A.
A1  - Benkhali, Faical  Ait
A1  - Akhperjanian, A. G.
A1  - Angüner, Ekrem Oǧuzhan
A1  - Anton, Gisela
A1  - Balenderan, Shangkari
A1  - Balzer, Arnim
A1  - Barnacka, Anna
A1  - Becherini, Yvonne
A1  - Tjus, J. Becker
A1  - Bernlöhr, K.
A1  - Birsin, E.
A1  - Bissaldi, E.
A1  - Biteau, Jonathan
A1  - Boettcher, Markus
A1  - Boisson, Catherine
A1  - Bolmont, J.
A1  - Bordas, Pol
A1  - Brucker, J.
A1  - Brun, Francois
A1  - Brun, Pierre
A1  - Bulik, Tomasz
A1  - Carrigan, Svenja
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chadwick, Paula M.
A1  - Chalme-Calvet, R.
A1  - Chaves, Ryan C. G.
A1  - Cheesebrough, A.
A1  - Chretien, M.
A1  - Colafrancesco, Sergio
A1  - Cologna, Gabriele
A1  - Conrad, Jan
A1  - Couturier, C.
A1  - Cui, Y.
A1  - Dalton, M.
A1  - Daniel, M. K.
A1  - Davids, I. D.
A1  - Degrange, B.
A1  - Deil, C.
A1  - deWilt, P.
A1  - Dickinson, H. J.
A1  - Djannati-Ataï, A.
A1  - Domainko, W.
A1  - Dubus, G.
A1  - Dutson, K.
A1  - Dyks, J.
A1  - Dyrda, M.
A1  - Edwards, T.
A1  - Egberts, Kathrin
A1  - Eger, P.
A1  - Espigat, P.
A1  - Farnier, C.
A1  - Fegan, S.
A1  - Feinstein, F.
A1  - Fernandes, M. V.
A1  - Fernandez, D.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Foerster, A.
A1  - Fuessling, M.
A1  - Gajdus, M.
A1  - Gallant, Y. A.
A1  - Garrigoux, T.
A1  - Giavitto, G.
A1  - Giebels, B.
A1  - Glicenstein, J. F.
A1  - Grondin, M. -H.
A1  - Grudzinska, M.
A1  - Haeffner, S.
A1  - Hahn, J.
A1  - Harris, J.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hervet, O.
A1  - Hillert, A.
A1  - Hinton, James Anthony
A1  - Hofmann, W.
A1  - Hofverberg, P.
A1  - Holler, M.
A1  - Horns, D.
A1  - Jacholkowska, A.
A1  - Jahn, C.
A1  - Jamrozy, M.
A1  - Janiak, M.
A1  - Jankowsky, F.
A1  - Jung, I.
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katz, U.
A1  - Kaufmann, S.
A1  - Khelifi, B.
A1  - Kieffer, M.
A1  - Klepser, S.
A1  - Klochkov, D.
A1  - Kluzniak, W.
A1  - Kneiske, T.
A1  - Kolitzus, D.
A1  - Komin, Nu.
A1  - Kosack, K.
A1  - Krakau, S.
A1  - Krayzel, F.
A1  - Krueger, P. P.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lefaucheur, J.
A1  - Lemiere, A.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J. -P.
A1  - Lennarz, D.
A1  - Lohse, T.
A1  - Lopatin, A.
A1  - Lu, C. -C.
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Marx, R.
A1  - Maurin, G.
A1  - Maxted, N.
A1  - Mayer, Michael
A1  - McComb, T. J. L.
A1  - Mehault, J.
A1  - Meintjes, P. J.
A1  - Menzler, U.
A1  - Meyer, M.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Moulin, Emmanuel
A1  - Murach, T.
A1  - Naumann, C. L.
A1  - de Naurois, M.
A1  - Niemiec, J.
A1  - Nolan, S. J.
A1  - Oakes, L.
A1  - Ohm, S.
A1  - Wilhelmi, E. de Ona
A1  - Opitz, B.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Arribas, M. Paz
A1  - Pekeur, N. W.
A1  - Pelletier, G.
A1  - Perez, J.
A1  - Petrucci, P. -O.
A1  - Peyaud, B.
A1  - Pita, S.
A1  - Poon, H.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Raue, M.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - de los Reyes, R.
A1  - Rieger, F.
A1  - Rob, L.
A1  - Romoli, C.
A1  - Rosier-Lees, S.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Sahakian, V.
A1  - Sanchez, David M.
A1  - Santangelo, Andrea
A1  - Schlickeiser, R.
A1  - Schuessler, F.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwarzburg, S.
A1  - Schwemmer, S.
A1  - Sol, H.
A1  - Spengler, G.
A1  - Spies, F.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Stinzing, F.
A1  - Stycz, K.
A1  - Sushch, Iurii
A1  - Szostek, A.
A1  - Tavernet, J. -P.
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Valerius, K.
A1  - van Eldik, C.
A1  - van Soelen, B.
A1  - Vasileiadis, G.
A1  - Venter, C.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voelk, H. J.
A1  - Volpe, F.
A1  - Vorster, M.
A1  - Vuillaume, T.
A1  - Wagner, S. J.
A1  - Wagner, P.
A1  - Ward, M.
A1  - Weidinger, M.
A1  - Weitzel, Q.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Willmann, P.
A1  - Woernlein, A.
A1  - Wouters, D.
A1  - Zabalza, V.
A1  - Zacharias, M.
A1  - Zajczyk, A.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zechlin, H. -S.
T1  - HESS J1640-465 - an exceptionally luminous TeV gamma-ray supernova remnant (vol 439, pg 2828, 2014)
T2  - Monthly notices of the Royal Astronomical Society
KW  - errata, addenda
KW  - radiation mechanisms: non-thermal
KW  - ISM: individual objects: G338.3-0.0
KW  - ISM: supernova remnants
Y1  - 2014
U6  - https://doi.org/10.1093/mnras/stu826
SN  - 0035-8711
SN  - 1365-2966
VL  - 441
IS  - 4
SP  - 3640
EP  - 3642
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Abramowski, Attila
A1  - Acero, F.
A1  - Aharonian, Felix A.
A1  - Akhperjanian, A. G.
A1  - Anton, Gisela
A1  - Balenderan, Shangkari
A1  - Balzer, Arnim
A1  - Barnacka, Anna
A1  - Becherini, Yvonne
A1  - Tjus, J. Becker
A1  - Bernlöhr, K.
A1  - Birsin, E.
A1  - Biteau, Jonathan
A1  - Bochow, A.
A1  - Boisson, Catherine
A1  - Bolmont, J.
A1  - Bordas, Pol
A1  - Brucker, J.
A1  - Brun, Francois
A1  - Brun, Pierre
A1  - Bulik, Tomasz
A1  - Carrigan, Svenja
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chadwick, Paula M.
A1  - Chaves, Ryan C. G.
A1  - Cheesebrough, A.
A1  - Colafrancesco, Sergio
A1  - Cologna, Gabriele
A1  - Conrad, Jan
A1  - Couturier, C.
A1  - Dalton, M.
A1  - Daniel, M. K.
A1  - Davids, I. D.
A1  - Degrange, B.
A1  - Deil, C.
A1  - deWilt, P.
A1  - Dickinson, H. J.
A1  - Djannati-Ataï, A.
A1  - Domainko, W.
A1  - Drury, L. O'C.
A1  - Dubus, G.
A1  - Dutson, K.
A1  - Dyks, J.
A1  - Dyrda, M.
A1  - Egberts, Kathrin
A1  - Eger, P.
A1  - Espigat, P.
A1  - Fallon, L.
A1  - Farnier, C.
A1  - Fegan, S.
A1  - Feinstein, F.
A1  - Fernandes, M. V.
A1  - Fernandez, D.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Foerster, A.
A1  - Fussling, Matthias
A1  - Gajdus, M.
A1  - Gallant, Y. A.
A1  - Garrigoux, T.
A1  - Gast, H.
A1  - Giebels, B.
A1  - Glicenstein, J. F.
A1  - Glueck, B.
A1  - Goering, D.
A1  - Grondin, M. -H.
A1  - Haeffner, S.
A1  - Hague, J. D.
A1  - Hahn, J.
A1  - Hampf, D.
A1  - Harris, J.
A1  - Heinz, S.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hillert, A.
A1  - Hinton, James Anthony
A1  - Hofmann, W.
A1  - Hofverberg, P.
A1  - Holler, M.
A1  - Horns, D.
A1  - Jacholkowska, A.
A1  - Jahn, C.
A1  - Jamrozy, M.
A1  - Jung, I.
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katz, U.
A1  - Kaufmann, S.
A1  - Khelifi, B.
A1  - Klepser, S.
A1  - Klochkov, D.
A1  - Kluzniak, W.
A1  - Kneiske, T.
A1  - Komin, Nu
A1  - Kosack, K.
A1  - Kossakowski, R.
A1  - Krayzel, F.
A1  - Krueger, P. P.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lefaucheur, J.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J. -P.
A1  - Lennarz, D.
A1  - Lohse, T.
A1  - Lopatin, A.
A1  - Lu, C. -C.
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Masbou, J.
A1  - Maurin, G.
A1  - Maxted, N.
A1  - Mayer, M.
A1  - McComb, T. J. L.
A1  - Medina, M. C.
A1  - Mehault, J.
A1  - Menzler, U.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Moulin, Emmanuel
A1  - Naumann, C. L.
A1  - Naumann-Godo, M.
A1  - de Naurois, M.
A1  - Nedbal, D.
A1  - Nekrassov, D.
A1  - Nguyen, N.
A1  - Niemiec, J.
A1  - Nolan, S. J.
A1  - Ohm, S.
A1  - Awilhelmi, E. de Ona
A1  - Opitz, B.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Arribas, M. Paz
A1  - Pekeur, N. W.
A1  - Pelletier, G.
A1  - Perez, J.
A1  - Petrucci, P. -O.
A1  - Peyaud, B.
A1  - Pita, S.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raue, M.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - de los Reyes, R.
A1  - Rieger, F.
A1  - Ripken, J.
A1  - Rob, L.
A1  - Rosier-Lees, S.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Sahakian, V.
A1  - Sanchez, David M.
A1  - Santangelo, Andrea
A1  - Schlickeiser, R.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwarzburg, S.
A1  - Schwemmer, S.
A1  - Sheidaei, F.
A1  - Skilton, J. L.
A1  - Sol, H.
A1  - Spengler, G.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Stinzing, F.
A1  - Stycz, K.
A1  - Sushch, Iurii
A1  - Szostek, A.
A1  - Tavernet, J. -P.
A1  - Terrier, R.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Valerius, K.
A1  - van Eldik, C.
A1  - Vasileiadis, G.
A1  - Venter, C.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Voelk, H. J.
A1  - Volpe, F.
A1  - Vorobiov, S.
A1  - Vorster, M.
A1  - Wagner, S. J.
A1  - Ward, M.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Wouters, D.
A1  - Zacharias, M.
A1  - Zajczyk, A.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zechlin, H. -S.
T1  - Search for Photon-Linelike Signatures from Dark Matter Annihilations with H.E.S.S.
JF  - Physical review letters
N2  - Gamma-ray line signatures can be expected in the very-high-energy (E-gamma > 100 GeV) domain due to self-annihilation or decay of dark matter (DM) particles in space. Such a signal would be readily distinguishable from astrophysical gamma-ray sources that in most cases produce continuous spectra that span over several orders of magnitude in energy. Using data collected with the H. E. S. S. gamma-ray instrument, upper limits on linelike emission are obtained in the energy range between similar to 500 GeV and similar to 25 TeV for the central part of the Milky Way halo and for extragalactic observations, complementing recent limits obtained with the Fermi-LAT instrument at lower energies. No statistically significant signal could be found. For monochromatic gamma-ray line emission, flux limits of (2 x 10(-7)-2 x 10(-5)) m(-2)s(-1)sr(-1) and (1 x 10(-8)- 2 x 10(-6)) m(-2)s(-1)sr(-1) are obtained for the central part of the Milky Way halo and extragalactic observations, respectively. For a DM particle mass of 1 TeV, limits on the velocity- averaged DM annihilation cross section <sigma upsilon >(chi chi ->gamma gamma) reach similar to 10(-27)cm(3)s(-1), based on the Einasto parametrization of the Galactic DM halo density profile. DOI: 10.1103/PhysRevLett.110.041301
Y1  - 2013
U6  - https://doi.org/10.1103/PhysRevLett.110.041301
SN  - 0031-9007
VL  - 110
IS  - 4
PB  - American Physical Society
CY  - College Park
ER  - 
TY  - JOUR
A1  - De Angelis, A.
A1  - Tatischeff, V.
A1  - Grenier, I. A.
A1  - McEnery, J.
A1  - Mallamaci, Manuela
A1  - Tavani, M.
A1  - Oberlack, U.
A1  - Hanlon, L.
A1  - Walter, R.
A1  - Argan, A.
A1  - Von Ballmoos, P.
A1  - Bulgarelli, A.
A1  - Bykov, A.
A1  - Hernanz, M.
A1  - Kanbach, G.
A1  - Kuvvetli, I.
A1  - Pearce, M.
A1  - Zdziarski, A.
A1  - Conrad, J.
A1  - Ghisellini, G.
A1  - Harding, A.
A1  - Isern, J.
A1  - Leising, M.
A1  - Longo, F.
A1  - Madejski, G.
A1  - Martinez, M.
A1  - Mazziotta, Mario Nicola
A1  - Paredes, J. M.
A1  - Pohl, Martin
A1  - Rando, R.
A1  - Razzano, M.
A1  - Aboudan, A.
A1  - Ackermann, M.
A1  - Addazi, A.
A1  - Ajello, M.
A1  - Albertus, C.
A1  - Alvarez, J. M.
A1  - Ambrosi, G.
A1  - Anton, S.
A1  - Antonelli, L. A.
A1  - Babic, A.
A1  - Baibussinov, B.
A1  - Balbom, M.
A1  - Baldini, L.
A1  - Balman, S.
A1  - Bambi, C.
A1  - Barres de Almeida, U.
A1  - Barrio, J. A.
A1  - Bartels, R.
A1  - Bastieri, D.
A1  - Bednarek, W.
A1  - Bernard, D.
A1  - Bernardini, E.
A1  - Bernasconi, T.
A1  - Bertucci, B.
A1  - Biland, A.
A1  - Bissaldi, E.
A1  - Boettcher, M.
A1  - Bonvicini, V.
A1  - Bosch-Ramon, V.
A1  - Bottacini, E.
A1  - Bozhilov, V.
A1  - Bretz, T.
A1  - Branchesi, M.
A1  - Brdar, V.
A1  - Bringmann, T.
A1  - Brogna, A.
A1  - Jorgensen, C. Budtz
A1  - Busetto, G.
A1  - Buson, S.
A1  - Busso, M.
A1  - Caccianiga, A.
A1  - Camera, S.
A1  - Campana, R.
A1  - Caraveo, P.
A1  - Cardillo, M.
A1  - Carlson, P.
A1  - Celestin, S.
A1  - Cermeno, M.
A1  - Chen, A.
A1  - Cheung, C. C.
A1  - Churazov, E.
A1  - Ciprini, S.
A1  - Coc, A.
A1  - Colafrancesco, S.
A1  - Coleiro, A.
A1  - Collmar, W.
A1  - Coppi, P.
A1  - Curado da Silva, R.
A1  - Cutini, S.
A1  - De Lotto, B.
A1  - de Martino, D.
A1  - De Rosa, A.
A1  - Del Santo, M.
A1  - Delgado, L.
A1  - Diehl, R.
A1  - Dietrich, S.
A1  - Dolgov, A. D.
A1  - Dominguez, A.
A1  - Prester, D. Dominis
A1  - Donnarumma, I.
A1  - Dorner, D.
A1  - Doro, M.
A1  - Dutra, M.
A1  - Elsaesser, D.
A1  - Fabrizio, M.
A1  - Fernandez-Barral, A.
A1  - Fioretti, V.
A1  - Foffano, L.
A1  - Formato, V.
A1  - Fornengo, N.
A1  - Foschini, L.
A1  - Franceschini, A.
A1  - Franckowiak, A.
A1  - Funk, S.
A1  - Fuschino, F.
A1  - Gaggero, D.
A1  - Galanti, G.
A1  - Gargano, F.
A1  - Gasparrini, D.
A1  - Gehrz, R.
A1  - Giammaria, P.
A1  - Giglietto, N.
A1  - Giommi, P.
A1  - Giordano, F.
A1  - Giroletti, M.
A1  - Ghirlanda, G.
A1  - Godinovic, N.
A1  - Gouiffes, C.
A1  - Grove, J. E.
A1  - Hamadache, C.
A1  - Hartmann, D. H.
A1  - Hayashida, M.
A1  - Hryczuk, A.
A1  - Jean, P.
A1  - Johnson, T.
A1  - Jose, J.
A1  - Kaufmann, S.
A1  - Khelifi, B.
A1  - Kiener, J.
A1  - Knodlseder, J.
A1  - Kolem, M.
A1  - Kopp, J.
A1  - Kozhuharov, V.
A1  - Labanti, C.
A1  - Lalkovski, S.
A1  - Laurent, P.
A1  - Limousin, O.
A1  - Linares, M.
A1  - Lindfors, E.
A1  - Lindner, M.
A1  - Liu, J.
A1  - Lombardi, S.
A1  - Loparco, F.
A1  - Lopez-Coto, R.
A1  - Lopez Moya, M.
A1  - Lott, B.
A1  - Lubrano, P.
A1  - Malyshev, D.
A1  - Mankuzhiyil, N.
A1  - Mannheim, K.
A1  - Marcha, M. J.
A1  - Marciano, A.
A1  - Marcote, B.
A1  - Mariotti, M.
A1  - Marisaldi, M.
A1  - McBreen, S.
A1  - Mereghetti, S.
A1  - Merle, A.
A1  - Mignani, R.
A1  - Minervini, G.
A1  - Moiseev, A.
A1  - Morselli, A.
A1  - Moura, F.
A1  - Nakazawa, K.
A1  - Nava, L.
A1  - Nieto, D.
A1  - Orienti, M.
A1  - Orio, M.
A1  - Orlando, E.
A1  - Orleanski, P.
A1  - Paiano, S.
A1  - Paoletti, R.
A1  - Papitto, A.
A1  - Pasquato, M.
A1  - Patricelli, B.
A1  - Perez-Garcia, M. A.
A1  - Persic, M.
A1  - Piano, G.
A1  - Pichel, A.
A1  - Pimenta, M.
A1  - Pittori, C.
A1  - Porter, T.
A1  - Poutanen, J.
A1  - Prandini, E.
A1  - Prantzos, N.
A1  - Produit, N.
A1  - Profumo, S.
A1  - Queiroz, F. S.
A1  - Raino, S.
A1  - Raklev, A.
A1  - Regis, M.
A1  - Reichardt, I.
A1  - Rephaeli, Y.
A1  - Rico, J.
A1  - Rodejohann, W.
A1  - Fernandez, G. Rodriguez
A1  - Roncadelli, M.
A1  - Roso, L.
A1  - Rovero, A.
A1  - Ruffini, R.
A1  - Sala, G.
A1  - Sanchez-Conde, M. A.
A1  - Santangelo, Andrea
A1  - Parkinson, P. Saz
A1  - Sbarrato, T.
A1  - Shearer, A.
A1  - Shellard, R.
A1  - Short, K.
A1  - Siegert, T.
A1  - Siqueira, C.
A1  - Spinelli, P.
A1  - Stamerra, A.
A1  - Starrfield, S.
A1  - Strong, A.
A1  - Strumke, I.
A1  - Tavecchio, F.
A1  - Taverna, R.
A1  - Terzic, T.
A1  - Thompson, D. J.
A1  - Tibolla, O.
A1  - Torres, D. F.
A1  - Turolla, R.
A1  - Ulyanov, A.
A1  - Ursi, A.
A1  - Vacchi, A.
A1  - Van den Abeele, J.
A1  - Vankova-Kirilovai, G.
A1  - Venter, C.
A1  - Verrecchia, F.
A1  - Vincent, P.
A1  - Wang, X.
A1  - Weniger, C.
A1  - Wu, X.
A1  - Zaharijas, G.
A1  - Zampieri, L.
A1  - Zane, S.
A1  - Zimmer, S.
A1  - Zoglauer, A.
T1  - Science with e-ASTROGAM A space mission for MeV-GeV gamma-ray astrophysics
JF  - Journal of High Energy Astrophysics
Y1  - 2018
U6  - https://doi.org/10.1016/j.jheap.2018.07.001
SN  - 2214-4048
SN  - 2214-4056
VL  - 19
SP  - 1
EP  - 106
PB  - Elsevier
CY  - Amsterdam
ER  - 
TY  - JOUR
A1  - Cheng, Xin
A1  - Zhang, Jie
A1  - Kliem, Bernhard
A1  - Török, Tibor
A1  - Xing, Chen
A1  - Zhou, Zhenjun
A1  - Inhester, Bernd
A1  - Ding, Mingde
T1  - Initiation and early kinematic evolution of solar eruptions
JF  - The Astrophysical Journal
N2  - We investigate the initiation and early evolution of 12 solar eruptions, including six active-region hot channel and six quiescent filament eruptions, which were well observed by the Solar Dynamics Observatory, as well as by the Solar Terrestrial Relations Observatory for the latter. The sample includes one failed eruption and 11 coronal mass ejections, with velocities ranging from 493 to 2140 km s(-1). A detailed analysis of the eruption kinematics yields the following main results. (1) The early evolution of all events consists of a slow-rise phase followed by a main-acceleration phase, the height-time profiles of which differ markedly and can be best fit, respectively, by a linear and an exponential function. This indicates that different physical processes dominate in these phases, which is at variance with models that involve a single process. (2) The kinematic evolution of the eruptions tends to be synchronized with the flare light curve in both phases. The synchronization is often but not always close. A delayed onset of the impulsive flare phase is found in the majority of the filament eruptions (five out of six). This delay and its trend to be larger for slower eruptions favor ideal MHD instability models. (3) The average decay index at the onset heights of the main acceleration is close to the threshold of the torus instability for both groups of events (although, it is based on a tentative coronal field model for the hot channels), suggesting that this instability initiates and possibly drives the main acceleration.
KW  - solar coronal mass ejections
KW  - stellar coronal mass ejections
KW  - solar storm
Y1  - 2020
U6  - https://doi.org/10.3847/1538-4357/ab886a
SN  - 1055-6796
SN  - 1476-3540
VL  - 894
IS  - 2
SP  - 1
EP  - 20
PB  - Cambridge Scientific Publishers
CY  - Cambridge
ER  - 
TY  - THES
A1  - Ketzer, Laura
T1  - The impact of stellar activity evolution on atmospheric mass loss of young exoplanets
T1  - Der Einfluss der stellaren Aktivitätsentwicklung auf den atmosphärischen Massenverlust von jungen Exoplaneten
N2  - The increasing number of known exoplanets raises questions about their demographics and the mechanisms that shape planets into how we observe them today. Young planets in close-in orbits are exposed to harsh environments due to the host star being magnetically highly active, which results in high X-ray and extreme UV fluxes impinging on the planet. Prolonged exposure to this intense photoionizing radiation can cause planetary atmospheres to heat up, expand and escape into space via a hydrodynamic escape process known as photoevaporation. For super-Earth and sub-Neptune-type planets, this can even lead to the complete erosion of their primordial gaseous atmospheres. A factor of interest for this particular mass-loss process is the activity evolution of the host star. Stellar rotation, which drives the dynamo and with it the magnetic activity of a star, changes significantly over the stellar lifetime. This strongly affects the amount of high-energy radiation received by a planet as stars age. At a young age, planets still host warm and extended envelopes, making them particularly susceptible to atmospheric evaporation. Especially in the first gigayear, when X-ray and UV levels can be 100 - 10,000 times higher than for the present-day sun, the characteristics of the host star and the detailed evolution of its high-energy emission are of importance.
In this thesis, I study the impact of stellar activity evolution on the high-energy-induced atmospheric mass loss of young exoplanets. The PLATYPOS code was developed as part of this thesis to calculate photoevaporative mass-loss rates over time. The code, which couples parameterized planetary mass-radius relations with an analytical hydrodynamic escape model, was used, together with Chandra and eROSITA X-ray observations, to investigate the future mass loss of the two young multiplanet systems V1298 Tau and K2-198. Further, in a numerical ensemble study, the effect of a realistic spread of activity tracks on the small-planet radius gap was investigated for the first time. The works in this thesis show that for individual systems, in particular if planetary masses are unconstrained, the difference between a young host star following a low-activity track vs. a high-activity one can have major implications: the exact shape of the activity evolution can determine whether a planet can hold on to some of its atmosphere, or completely loses its envelope, leaving only the bare rocky core behind. For an ensemble of simulated planets, an observationally-motivated distribution of activity tracks does not substantially change the final radius distribution at ages of several gigayears. My simulations indicate that the overall shape and slope of the resulting small-planet radius gap is not significantly affected by the spread in stellar activity tracks. However, it can account for a certain scattering or fuzziness observed in and around the radius gap of the observed exoplanet population.
N2  - Die steigende Anzahl bekannter Exoplaneten wirft Fragen zu ihrer Demografie und den Mechanismen auf, die Planeten in ihre heutige beobachtete Form bringen. Junge Planeten, die sehr nah um ihren Wirtsstern kreisen, sind extremen Umgebungen ausgesetzt, da der Stern eine hohe magnetische Aktivität aufweist. Das führt wiederum dazu, dass der Planet einer enormen Röntgen- und Extrem-UV-Strahlung ausgesetzt ist. Ist der Planet über einen längeren Zeitraum dieser intensiven photoionisierenden Strahlung ausgesetzt, kann dies dazu führen, dass Planetenatmosphären sich aufheizen, ausdehnen und durch einen hydrodynamischen Entweichungsprozess namens Photoevaporation ins All entweichen, sozusagen verdampfen. Bei Planeten, in der Größenordnung von Super-Erden und Sub-Neptunen, kann dies sogar zur vollständigen Erosion ihrer Ur-Atmosphären führen. Ein interessanter Faktor, der für diesen  Massenverlustprozess eine Rolle spielt, ist die Aktivitätsentwicklung des Wirtssterns. Die Rotation eines Sterns, die den Dynamo und damit die magnetische Aktivität antreibt, ändert sich im Laufe der Lebensdauer eines Sterns erheblich. Dies hat einen starken Einfluss auf die Menge der hochenergetischen Strahlung, den ein Planet mit zunehmendem Alter des Sterns empfängt. In jungen Jahren besitzen Planeten noch warme und ausgedehnte Hüllen, was sie besonders anfällig für atmosphärische Verdunstung macht. Insbesondere in den ersten Gigajahren, wenn die Röntgen- und UV-Strahlung 100 - 10,000 Mal höher sein kann als bei der heutigen Sonne, sind die Eigenschaften des Wirtssterns und die detaillierte Entwicklung seiner hochenergetischen Emission von Bedeutung.

In dieser Arbeit untersuche ich die Auswirkungen der Entwicklung der stellaren Aktivität auf den durch hochenergetische Strahlung verursachten atmosphärischen Massenverlust junger Exoplaneten. Der PLATYPOS-Code wurde im Rahmen dieser Arbeit entwickelt, um die photoevaporativen Massenverlustraten für verschiedene stellare Alter zu berechnen. Der Code verknüpft parametrisierte Planetenmasse-Radius-Beziehungen mit einem analytischen Modell für den hydrodynamischen Massenverlust. Er wurde zusammen mit Chandra- und eROSITA-Röntgenbeobachtungen dazu verwendet, den zukünftigen Massenverlust der beiden jungen Mehrplanetensysteme V1298 Tau und K2-198 zu untersuchen. Darüber hinaus wurde in einer numerischen Ensemblestudie erstmals der Effekt einer realistischen Verteilung von stellaren Aktivitäts-Tracks auf das sogenannte Radius-Tal bei kleinen Planeten untersucht. Die Arbeiten in dieser Dissertation zeigen, dass für einzelne Systeme, insbesondere wenn die Planetenmassen unbestimmt sind, der Unterschied zwischen einem jungen Wirtsstern, der einem Track mit niedriger Aktivität gegenüber einem solchen mit hoher Aktivität folgt, gravierende Auswirkungen haben kann: Die genaue Form der Aktivitätsentwicklung kann darüber entscheiden, ob ein Planet einen Teil seiner Atmosphäre behält oder seine Hülle vollständig verliert und nur den nackten Gesteinskern behält. Für ein Ensemble von simulierten Planeten ändert eine durch Beobachtungen motivierte Verteilung von Aktivitäts-Tracks die endgültige Radiusverteilung der Planeten nach mehreren Gigajahren nicht wesentlich. Meine Simulationen deuten darauf hin, dass die Form und Steigung des sich ergebenden Radius-Tals bei Kleinplaneten nicht wesentlich von der Streuung der stellaren Aktivitäts-Tracks beeinflusst wird. Eine gewisse Streuung oder Unschärfe im Radius-Tal der beobachteten Exoplanetenpopulation kann damit allerdings durchaus erklärt werden.
KW  - Exoplaneten
KW  - star-planet interaction
KW  - stellar physics
KW  - exoplanets
KW  - exoplanet atmospheres
KW  - Sternphysik
KW  - Stern-Planeten-Wechselwirkung
KW  - Exoplanetenatmosphären
Y1  - 2024
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-626819
ER  - 
TY  - JOUR
A1  - Herzog, Marc
A1  - Reppert, Alexander von
A1  - Pudell, Jan-Etienne
A1  - Henkel, Carsten
A1  - Kronseder, Matthias
A1  - Back, Christian H.
A1  - Maznev, Alexei A.
A1  - Bargheer, Matias
T1  - Phonon-dominated energy transport in purely metallic heterostructures
JF  - Advanced functional materials
N2  - Ultrafast X-ray diffraction is used to quantify the transport of energy in laser-excited nanoscale gold-nickel (Au-Ni) bilayers. 
Electron transport and efficient electron-phonon coupling in Ni convert the laser-deposited energy in the conduction electrons within a few picoseconds into a strong non-equilibrium between hot Ni and cold Au phonons at the bilayer interface. 

Modeling of the subsequent equilibration dynamics within various two-temperature models confirms that for ultrathin Au films, the thermal transport is dominated by phonons instead of conduction electrons because of the weak electron-phonon coupling in Au.
KW  - heterostructures
KW  - nanoscale energy transports
KW  - non-equilibrium
KW  - thermal
KW  - transports
KW  - ultrafast phenomena
Y1  - 2022
U6  - https://doi.org/10.1002/adfm.202206179
SN  - 1616-301X
SN  - 1616-3028
VL  - 32
IS  - 41
PB  - Wiley-VCH
CY  - Weinheim
ER  - 
TY  - JOUR
A1  - Herbst, Konstantin
A1  - Baalmann, Lennart R.
A1  - Bykov, Andrei
A1  - Engelbrecht, N. Eugene
A1  - Ferreira, Stefan E. S.
A1  - Izmodenov, Vladislav V.
A1  - Korolkov, Sergey D.
A1  - Levenfish, Ksenia P.
A1  - Linsky, Jeffrey L.
A1  - Meyer, Dominique M. -A.
A1  - Scherer, Klaus
A1  - Strauss, R. Du Toit
T1  - Astrospheres of planet-hosting cool stars and beyond when modeling meets observations
JF  - Space science reviews
N2  - Thanks to dedicated long-term missions like Voyager and GOES over the past 50 years, much insight has been gained on the activity of our Sun, the solar wind, its interaction with the interstellar medium, and, thus, about the formation, the evolution, and the structure of the heliosphere. Additionally, with the help of multi-wavelength observations by the Hubble Space Telescope, Kepler, and TESS, we not only were able to detect a variety of extrasolar planets and exomoons but also to study the characteristics of their host stars, and thus became aware that other stars drive bow shocks and astrospheres. Although features like, e.g., stellar winds, could not be measured directly, over the past years several techniques have been developed allowing us to indirectly derive properties like stellar mass-loss rates and stellar wind speeds, information that can be used as direct input to existing astrospheric modeling codes. In this review, the astrospheric modeling efforts of various stars will be presented. Starting with the heliosphere as a benchmark of astrospheric studies, investigating the paleo-heliospheric changes and the Balmer H alpha projections to 1 pc, we investigate the surroundings of cool and hot stars, but also of more exotic objects like neutron stars. While pulsar wind nebulae (PWNs) might be a source of high-energy galactic cosmic rays (GCRs), the astrospheric environments of cool and hot stars form a natural shield against GCRs. Their modulation within these astrospheres, and the possible impact of turbulence, are also addressed. This review shows that all of the presented modeling efforts are in excellent agreement with currently available observations.
KW  - Magneto-hydrodynamic modeling
KW  - Stochastic differential equations
KW  - Galactic cosmic rays
KW  - Heliosphere
KW  - Astrosphere
Y1  - 2022
U6  - https://doi.org/10.1007/s11214-022-00894-3
SN  - 0038-6308
SN  - 1572-9672
VL  - 218
IS  - 4
PB  - Springer Nature
CY  - Dordrecht
ER  - 
TY  - JOUR
A1  - Bojahr, Andre
A1  - Gohlke, Matthias
A1  - Leitenberger, Wolfram
A1  - Pudell, Jan-Etienne
A1  - Reinhardt, Matthias
A1  - Reppert, Alexander von
A1  - Rössle, Matthias
A1  - Sander, Mathias
A1  - Gaal, Peter
A1  - Bargheer, Matias
T1  - Second Harmonic Generation of Nanoscale Phonon Wave Packets
JF  - Physical review letters
N2  - Phonons are often regarded as delocalized quasiparticles with certain energy and momentum. The anharmonic interaction of phonons determines macroscopic properties of the solid, such as thermal expansion or thermal conductivity, and a detailed understanding becomes increasingly important for functional nanostructures. Although phonon-phonon scattering processes depicted in simple wave-vector diagrams are the basis of theories describing these macroscopic phenomena, experiments directly accessing these coupling channels are scarce. We synthesize monochromatic acoustic phonon wave packets with only a few cycles to introduce nonlinear phononics as the acoustic counterpart to nonlinear optics. Control of the wave vector, bandwidth, and consequently spatial extent of the phonon wave packets allows us to observe nonlinear phonon interaction, in particular, second harmonic generation, in real time by wave-vector-sensitive Brillouin scattering with x-rays and optical photons.
Y1  - 2015
U6  - https://doi.org/10.1103/PhysRevLett.115.195502
SN  - 0031-9007
SN  - 1079-7114
VL  - 115
IS  - 19
PB  - American Physical Society
CY  - College Park
ER  - 
TY  - JOUR
A1  - Willig, Lisa
A1  - Reppert, Alexander von
A1  - Deb, Marwan
A1  - Ganss, F.
A1  - Hellwig, O.
A1  - Bargheer, Matias
T1  - Finite-size effects in ultrafast remagnetization dynamics of FePt
JF  - Physical review : B, Condensed matter and materials physics
N2  - We investigate the ultrafast magnetization dynamics of FePt in the L1(0) phase after an optical heating pulse, as used in heat-assisted magnetic recording. We compare continuous and nano-granular thin films and emphasize the impact of the finite size on the remagnetization dynamics. The remagnetization speeds up significantly with increasing external magnetic field only for the continuous film, where domain-wall motion governs the dynamics. The ultrafast remagnetization dynamics in the continuous film are only dominated by heat transport in the regime of high magnetic fields, whereas the timescale required for cooling is prevalent in the granular film for all magnetic field strengths. These findings highlight the necessary conditions for studying the intrinsic heat transport properties in magnetic materials.
Y1  - 2019
U6  - https://doi.org/10.1103/PhysRevB.100.224408
SN  - 2469-9950
SN  - 2469-9969
VL  - 100
IS  - 22
PB  - American Physical Society
CY  - College Park
ER  - 
TY  - JOUR
A1  - Koc, A.
A1  - Reinhardt, M.
A1  - Reppert, Alexander von
A1  - Rössle, Matthias
A1  - Leitenberger, Wolfram
A1  - Gleich, M.
A1  - Weinelt, M.
A1  - Zamponi, Flavio
A1  - Bargheer, Matias
T1  - Grueneisen-approach for the experimental determination of transient spin and phonon energies from ultrafast x-ray diffraction data: gadolinium
JF  - Journal of physics : Condensed matter
N2  - We study gadolinium thin films as a model system for ferromagnets with negative thermal expansion. Ultrashort laser pulses heat up the electronic subsystem and we follow the transient strain via ultrafast x-ray diffraction. In terms of a simple Grueneisen approach, the strain is decomposed into two contributions proportional to the thermal energy of spin and phonon subsystems. Our analysis reveals that upon femtosecond laser excitation, phonons and spins can be driven out of thermal equilibrium for several nanoseconds.
KW  - ultrafast
KW  - x-ray diffraction
KW  - magnetostriction
KW  - nonequilibrium
KW  - spin
KW  - phonon
KW  - rare earth
Y1  - 2017
U6  - https://doi.org/10.1088/1361-648X/aa7187
SN  - 0953-8984
SN  - 1361-648X
VL  - 29
SP  - 5884
EP  - 5891
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  - 
TY  - JOUR
A1  - Cervantes Villa, Juan Sebastian
A1  - Shprits, Yuri Y.
A1  - Aseev, Nikita
A1  - Allison, Hayley J.
T1  - Quantifying the effects of EMIC wave scattering and magnetopause shadowing in the outer electron radiation belt by means of data assimilation
JF  - Journal of geophysical research : Space physics
N2  - In this study we investigate two distinct loss mechanisms responsible for the rapid dropouts of radiation belt electrons by assimilating data from Van Allen Probes A and B and Geostationary Operational Environmental Satellites (GOES) 13 and 15 into a 3-D diffusion model. In particular, we examine the respective contribution of electromagnetic ion cyclotron (EMIC) wave scattering and magnetopause shadowing for values of the first adiabatic invariant mu ranging from 300 to 3,000 MeV G(-1). We inspect the innovation vector and perform a statistical analysis to quantitatively assess the effect of both processes as a function of various geomagnetic indices, solar wind parameters, and radial distance from the Earth. Our results are in agreement with previous studies that demonstrated the energy dependence of these two mechanisms. We show that EMIC wave scattering tends to dominate loss at lower L shells, and it may amount to between 10%/hr and 30%/hr of the maximum value of phase space density (PSD) over all L shells for fixed first and second adiabatic invariants. On the other hand, magnetopause shadowing is found to deplete electrons across all energies, mostly at higher L shells, resulting in loss from 50%/hr to 70%/hr of the maximum PSD. Nevertheless, during times of enhanced geomagnetic activity, both processes can operate beyond such location and encompass the entire outer radiation belt.
Y1  - 2020
U6  - https://doi.org/10.1029/2020JA028208
SN  - 2169-9380
SN  - 2169-9402
VL  - 125
IS  - 8
PB  - American Geophysical Union
CY  - Washington
ER  - 
TY  - INPR
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A1  - Papyan, G.
A1  - Paredes, J. M.
A1  - Pareschi, G.
A1  - Parks, G.
A1  - Parraud, J. -M.
A1  - Parsons, D.
A1  - Arribas, M. Paz
A1  - Pech, M.
A1  - Pedaletti, G.
A1  - Pelassa, V.
A1  - Pelat, D.
A1  - Perez, M. D. C.
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A1  - Petrucci, P-O
A1  - Peyaud, B.
A1  - Pichel, A.
A1  - Pita, S.
A1  - Pizzolato, F.
A1  - Platos, L.
A1  - Platzer, R.
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A1  - Pohl, M.
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A1  - Ponz, J. D.
A1  - Potter, W.
A1  - Poutanen, J.
A1  - Prandini, E.
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A1  - Prouza, M.
A1  - Proyetti, M.
A1  - Puerto-Gimenez, I.
A1  - Puehlhofer, G.
A1  - Puljak, I.
A1  - Punch, M.
A1  - Pyziol, R.
A1  - Quel, E. J.
A1  - Quinn, J.
A1  - Quirrenbach, A.
A1  - Racero, E.
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A1  - Ramon, P.
A1  - Rando, R.
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A1  - Rataj, M.
A1  - Raue, M.
A1  - Reardon, P.
A1  - Reimann, O.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Reitberger, K.
A1  - Renaud, M.
A1  - Renner, S.
A1  - Reville, B.
A1  - Rhode, W.
A1  - Ribo, M.
A1  - Ribordy, M.
A1  - Richer, M. G.
A1  - Rico, J.
A1  - Ridky, J.
A1  - Rieger, F.
A1  - Ringegni, P.
A1  - Ripken, J.
A1  - Ristori, P. R.
A1  - Riviere, A.
A1  - Rivoire, S.
A1  - Rob, L.
A1  - Roeser, U.
A1  - Rohlfs, R.
A1  - Rojas, G.
A1  - Romano, Patrizia
A1  - Romaszkan, W.
A1  - Romero, G. E.
A1  - Rosen, S.
A1  - Lees, S. Rosier
A1  - Ross, D.
A1  - Rouaix, G.
A1  - Rousselle, J.
A1  - Rousselle, S.
A1  - Rovero, A. C.
A1  - Roy, F.
A1  - Royer, S.
A1  - Rudak, B.
A1  - Rulten, C.
A1  - Rupinski, M.
A1  - Russo, F.
A1  - Ryde, F.
A1  - Sacco, B.
A1  - Saemann, E. O.
A1  - Saggion, A.
A1  - Safiakian, V.
A1  - Saito, K.
A1  - Saito, T.
A1  - Saito, Y.
A1  - Sakaki, N.
A1  - Sakonaka, R.
A1  - Salini, A.
A1  - Sanchez, F.
A1  - Sanchez-Conde, M.
A1  - Sandoval, A.
A1  - Sandaker, H.
A1  - Sant'Ambrogio, E.
A1  - Santangelo, Andrea
A1  - Santos, E. M.
A1  - Sanuy, A.
A1  - Sapozhnikov, L.
A1  - Sarkar, S.
A1  - Sartore, N.
A1  - Sasaki, H.
A1  - Satalecka, K.
A1  - Sawada, M.
A1  - Scalzotto, V.
A1  - Scapin, V.
A1  - Scarcioffolo, M.
A1  - Schafer, J.
A1  - Schanz, T.
A1  - Schlenstedt, S.
A1  - Schlickeiser, R.
A1  - Schmidt, T.
A1  - Schmoll, J.
A1  - Schovanek, P.
A1  - Schroedter, M.
A1  - Schultz, C.
A1  - Schultze, J.
A1  - Schulz, A.
A1  - Schure, K.
A1  - Schwab, T.
A1  - Schwanke, U.
A1  - Schwarz, J.
A1  - Schwarzburg, S.
A1  - Schweizer, T.
A1  - Schwemmer, S.
A1  - Segreto, A.
A1  - Seiradakis, J. -H.
A1  - Sembroski, G. H.
A1  - Seweryn, K.
A1  - Sharma, M.
A1  - Shayduk, M.
A1  - Shellard, R. C.
A1  - Shi, J.
A1  - Shibata, T.
A1  - Shibuya, A.
A1  - Shum, E.
A1  - Sidoli, L.
A1  - Sidz, M.
A1  - Sieiro, J.
A1  - Sikora, M.
A1  - Silk, J.
A1  - Sillanpaa, A.
A1  - Singh, B. B.
A1  - Sitarek, J.
A1  - Skole, C.
A1  - Smareglia, R.
A1  - Smith, A.
A1  - Smith, D.
A1  - Smith, J.
A1  - Smith, N.
A1  - Sobczynska, D.
A1  - Sol, H.
A1  - Sottile, G.
A1  - Sowinski, M.
A1  - Spanier, F.
A1  - Spiga, D.
A1  - Spyrou, S.
A1  - Stamatescu, V.
A1  - Stamerra, A.
A1  - Starling, R.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Steiner, S.
A1  - Stergioulas, N.
A1  - Sternberger, R.
A1  - Sterzel, M.
A1  - Stinzing, F.
A1  - Stodulski, M.
A1  - Straumann, U.
A1  - Strazzeri, E.
A1  - Stringhetti, L.
A1  - Suarez, A.
A1  - Suchenek, M.
A1  - Sugawara, R.
A1  - Sulanke, K. -H.
A1  - Sun, S.
A1  - Supanitsky, A. D.
A1  - Suric, T.
A1  - Sutcliffe, P.
A1  - Sykes, J.
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A1  - Tagliaferri, G.
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A1  - Takahashi, H.
A1  - Takahashi, K.
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A1  - Talbot, C.
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A1  - Tanaka, M.
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A1  - Tasan, J.
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A1  - Telezhinsky, Igor O.
A1  - Temnikov, P.
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A1  - Tibaldo, L.
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A1  - Uslenghi, M.
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A1  - van Eldik, C.
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A1  - Werner, M.
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A1  - White, R.
A1  - Wierzcholska, A.
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A1  - Yoshikoshi, T.
A1  - Zabalza, V.
A1  - Zacharias, M.
A1  - Zajczyk, A.
A1  - Zanin, R.
A1  - Zdziarski, A.
A1  - Zech, Alraune
A1  - Zhao, A.
A1  - Zhou, X.
A1  - Zietara, K.
A1  - Ziolkowski, J.
A1  - Ziolkowski, P.
A1  - Zitelli, V.
A1  - Zurbach, C.
A1  - Zychowski, P.
T1  - Introducing the CTA concept
T2  - Astroparticle physics
N2  - The Cherenkov Telescope Array (CTA) is a new observatory for very high-energy (VHE) gamma rays. CTA has ambitions science goals, for which it is necessary to achieve full-sky coverage, to improve the sensitivity by about an order of magnitude, to span about four decades of energy, from a few tens of GeV to above 100 TeV with enhanced angular and energy resolutions over existing VHE gamma-ray observatories. An international collaboration has formed with more than 1000 members from 27 countries in Europe, Asia, Africa and North and South America. In 2010 the CTA Consortium completed a Design Study and started a three-year Preparatory Phase which leads to production readiness of CTA in 2014. In this paper we introduce the science goals and the concept of CTA, and provide an overview of the project.
KW  - TeV gamma-ray astronomy
KW  - Air showers
KW  - Cherenkov Telescopes
Y1  - 2013
U6  - https://doi.org/10.1016/j.astropartphys.2013.01.007
SN  - 0927-6505
SN  - 1873-2852
VL  - 43
IS  - 2
SP  - 3
EP  - 18
PB  - Elsevier
CY  - Amsterdam
ER  - 
TY  - JOUR
A1  - Warby, Jonathan
A1  - Zu, Fengshuo
A1  - Zeiske, Stefan
A1  - Gutierrez-Partida, Emilio
A1  - Frohloff, Lennart
A1  - Kahmann, Simon
A1  - Frohna, Kyle
A1  - Mosconi, Edoardo
A1  - Radicchi, Eros
A1  - Lang, Felix
A1  - Shah, Sahil
A1  - Pena-Camargo, Francisco
A1  - Hempel, Hannes
A1  - Unold, Thomas
A1  - Koch, Norbert
A1  - Armin, Ardalan
A1  - De Angelis, Filippo
A1  - Stranks, Samuel D.
A1  - Neher, Dieter
A1  - Stolterfoht, Martin
T1  - Understanding performance limiting interfacial recombination in pin Perovskite solar cells
JF  - Advanced energy materials
N2  - Perovskite semiconductors are an attractive option to overcome the limitations of established silicon based photovoltaic (PV) technologies due to their exceptional opto-electronic properties and their successful integration into multijunction cells. However, the performance of single- and multijunction cells is largely limited by significant nonradiative recombination at the perovskite/organic electron transport layer junctions. In this work, the cause of interfacial recombination at the perovskite/C-60 interface is revealed via a combination of photoluminescence, photoelectron spectroscopy, and first-principle numerical simulations. It is found that the most significant contribution to the total C-60-induced recombination loss occurs within the first monolayer of C-60, rather than in the bulk of C-60 or at the perovskite surface. The experiments show that the C-60 molecules act as deep trap states when in direct contact with the perovskite. It is further demonstrated that by reducing the surface coverage of C-60, the radiative efficiency of the bare perovskite layer can be retained. The findings of this work pave the way toward overcoming one of the most critical remaining performance losses in perovskite solar cells.
KW  - C60
KW  - defects
KW  - interface recombination
KW  - loss mechanisms
KW  - perovskites
KW  - solar cells
Y1  - 2022
U6  - https://doi.org/10.1002/aenm.202103567
SN  - 1614-6832
SN  - 1614-6840
VL  - 12
IS  - 12
PB  - Wiley-VCH
CY  - Weinheim
ER  - 
TY  - JOUR
A1  - Abramowski, Attila
A1  - Acero, F.
A1  - Aharonian, Felix A.
A1  - Akhperjanian, A. G.
A1  - Anton, Gisela
A1  - Balzer, Arnim
A1  - Barnacka, Anna
A1  - de Almeida, U. Barres
A1  - Becherini, Yvonne
A1  - Becker, J.
A1  - Behera, B.
A1  - Bernlöhr, K.
A1  - Birsin, E.
A1  - Biteau, Jonathan
A1  - Bochow, A.
A1  - Boisson, Catherine
A1  - Bolmont, J.
A1  - Bordas, Pol
A1  - Brucker, J.
A1  - Brun, Francois
A1  - Brun, Pierre
A1  - Bulik, Tomasz
A1  - Buesching, I.
A1  - Carrigan, Svenja
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chadwick, Paula M.
A1  - Charbonnier, A.
A1  - Chaves, Ryan C. G.
A1  - Cheesebrough, A.
A1  - Clapson, A. C.
A1  - Coignet, G.
A1  - Cologna, Gabriele
A1  - Conrad, Jan
A1  - Dalton, M.
A1  - Daniel, M. K.
A1  - Davids, I. D.
A1  - Degrange, B.
A1  - Deil, C.
A1  - Dickinson, H. J.
A1  - Djannati-Ataï, A.
A1  - Domainko, W.
A1  - Drury, L. O'C.
A1  - Dubus, G.
A1  - Dutson, K.
A1  - Dyks, J.
A1  - Dyrda, M.
A1  - Egberts, Kathrin
A1  - Eger, P.
A1  - Espigat, P.
A1  - Fallon, L.
A1  - Farnier, C.
A1  - Fegan, S.
A1  - Feinstein, F.
A1  - Fernandes, M. V.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Foerster, A.
A1  - Fuessling, M.
A1  - Gallant, Y. A.
A1  - Gast, H.
A1  - Gerard, L.
A1  - Gerbig, D.
A1  - Giebels, B.
A1  - Glicenstein, J. F.
A1  - Glueck, B.
A1  - Goret, P.
A1  - Goering, D.
A1  - Haeffner, S.
A1  - Hague, J. D.
A1  - Hampf, D.
A1  - Hauser, M.
A1  - Heinz, S.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hinton, James Anthony
A1  - Hoffmann, A.
A1  - Hofmann, W.
A1  - Hofverberg, P.
A1  - Holler, M.
A1  - Horns, D.
A1  - Jacholkowska, A.
A1  - de Jager, O. C.
A1  - Jahn, C.
A1  - Jamrozy, M.
A1  - Jung, I.
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katz, U.
A1  - Kaufmann, S.
A1  - Keogh, D.
A1  - Khangulyan, D.
A1  - Khelifi, B.
A1  - Klochkov, D.
A1  - Kluzniak, W.
A1  - Kneiske, T.
A1  - Komin, Nu.
A1  - Kosack, K.
A1  - Kossakowski, R.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lennarz, D.
A1  - Lohse, T.
A1  - Lopatin, A.
A1  - Lu, C. -C.
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Masbou, J.
A1  - Maurin, D.
A1  - Maxted, N.
A1  - Mayer, M.
A1  - McComb, T. J. L.
A1  - Medina, M. C.
A1  - Mehault, J.
A1  - Moderski, R.
A1  - Moulin, Emmanuel
A1  - Naumann, C. L.
A1  - Naumann-Godo, M.
A1  - de Naurois, M.
A1  - Nedbal, D.
A1  - Nekrassov, D.
A1  - Nguyen, N.
A1  - Nicholas, B.
A1  - Niemiec, J.
A1  - Nolan, S. J.
A1  - Ohm, S.
A1  - Wilhelmi, E. de Ona
A1  - Opitz, B.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Panter, M.
A1  - Arribas, M. Paz
A1  - Pedaletti, G.
A1  - Pelletier, G.
A1  - Petrucci, P. -O.
A1  - Pita, S.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raue, M.
A1  - Rayner, S. M.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - de los Reyes, R.
A1  - Rieger, F.
A1  - Ripken, J.
A1  - Rob, L.
A1  - Rosier-Lees, S.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Ruppel, J.
A1  - Sahakian, V.
A1  - Sanchez, David M.
A1  - Santangelo, Andrea
A1  - Schlickeiser, R.
A1  - Schoeck, F. M.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwarzburg, S.
A1  - Schwemmer, S.
A1  - Sheidaei, F.
A1  - Skilton, J. L.
A1  - Sol, H.
A1  - Spengler, G.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Stinzing, F.
A1  - Stycz, K.
A1  - Sushch, Iurii
A1  - Szostek, A.
A1  - Tavernet, J. -P.
A1  - Terrier, R.
A1  - Tluczykont, M.
A1  - Valerius, K.
A1  - van Eldik, C.
A1  - Vasileiadis, G.
A1  - Venter, C.
A1  - Vialle, J. P.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Voelk, H. J.
A1  - Volpe, F.
A1  - Vorobiov, S.
A1  - Vorster, M.
A1  - Wagner, S. J.
A1  - Ward, M.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Zacharias, M.
A1  - Zajczyk, A.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zechlin, H. -S.
A1  - Aleksic, J.
A1  - Antonelli, L. A.
A1  - Antoranz, P.
A1  - Backes, Michael
A1  - Barrio, J. A.
A1  - Bastieri, D.
A1  - Becerra Gonzalez, J.
A1  - Bednarek, W.
A1  - Berdyugin, A.
A1  - Berger, K.
A1  - Bernardini, E.
A1  - Biland, A.
A1  - Blanch Bigas, O.
A1  - Bock, R. K.
A1  - Boller, A.
A1  - Bonnoli, G.
A1  - Tridon, D. Borla
A1  - Braun, I.
A1  - Bretz, T.
A1  - Canellas, A.
A1  - Carmona, E.
A1  - Carosi, A.
A1  - Colin, P.
A1  - Colombo, E.
A1  - Contreras, J. L.
A1  - Cortina, J.
A1  - Cossio, L.
A1  - Covino, S.
A1  - Dazzi, F.
A1  - De Angelis, A.
A1  - De Cea del Pozo, E.
A1  - De Lotto, B.
A1  - Delgado Mendez, C.
A1  - Diago Ortega, A.
A1  - Doert, M.
A1  - Dominguez, A.
A1  - Prester, Dijana Dominis
A1  - Dorner, D.
A1  - Doro, M.
A1  - Elsaesser, D.
A1  - Ferenc, D.
A1  - Fonseca, M. V.
A1  - Font, L.
A1  - Fruck, C.
A1  - Garcia Lopez, R. J.
A1  - Garczarczyk, M.
A1  - Garrido, D.
A1  - Giavitto, G.
A1  - Godinovic, N.
A1  - Hadasch, D.
A1  - Haefner, D.
A1  - Herrero, A.
A1  - Hildebrand, D.
A1  - Hoehne-Moench, D.
A1  - Hose, J.
A1  - Hrupec, D.
A1  - Huber, B.
A1  - Jogler, T.
A1  - Klepser, S.
A1  - Kraehenbuehl, T.
A1  - Krause, J.
A1  - La Barbera, A.
A1  - Lelas, D.
A1  - Leonardo, E.
A1  - Lindfors, E.
A1  - Lombardi, S.
A1  - Lopez, M.
A1  - Lorenz, E.
A1  - Makariev, M.
A1  - Maneva, G.
A1  - Mankuzhiyil, N.
A1  - Mannheim, K.
A1  - Maraschi, L.
A1  - Mariotti, M.
A1  - Martinez, M.
A1  - Mazin, D.
A1  - Meucci, M.
A1  - Miranda, J. M.
A1  - Mirzoyan, R.
A1  - Miyamoto, H.
A1  - Moldon, J.
A1  - Moralejo, A.
A1  - Munar, P.
A1  - Nieto, D.
A1  - Nilsson, K.
A1  - Orito, R.
A1  - Oya, I.
A1  - Paneque, D.
A1  - Paoletti, R.
A1  - Pardo, S.
A1  - Paredes, J. M.
A1  - Partini, S.
A1  - Pasanen, M.
A1  - Pauss, F.
A1  - Perez-Torres, M. A.
A1  - Persic, M.
A1  - Peruzzo, L.
A1  - Pilia, M.
A1  - Pochon, J.
A1  - Prada, F.
A1  - Moroni, P. G. Prada
A1  - Prandini, E.
A1  - Puljak, I.
A1  - Reichardt, I.
A1  - Reinthal, R.
A1  - Rhode, W.
A1  - Ribo, M.
A1  - Rico, J.
A1  - Ruegamer, S.
A1  - Saggion, A.
A1  - Saito, K.
A1  - Saito, T. Y.
A1  - Salvati, M.
A1  - Satalecka, K.
A1  - Scalzotto, V.
A1  - Scapin, V.
A1  - Schultz, C.
A1  - Schweizer, T.
A1  - Shayduk, M.
A1  - Shore, S. N.
A1  - Sillanpaa, A.
A1  - Sitarek, J.
A1  - Sobczynska, D.
A1  - Spanier, F.
A1  - Spiro, S.
A1  - Stamerra, A.
A1  - Steinke, B.
A1  - Storz, J.
A1  - Strah, N.
A1  - Suric, T.
A1  - Takalo, L.
A1  - Takami, H.
A1  - Tavecchio, F.
A1  - Temnikov, P.
A1  - Terzic, T.
A1  - Tescaro, D.
A1  - Teshima, M.
A1  - Thom, M.
A1  - Tibolla, O.
A1  - Torres, D. F.
A1  - Treves, A.
A1  - Vankov, H.
A1  - Vogler, P.
A1  - Wagner, R. M.
A1  - Weitzel, Q.
A1  - Zabalza, V.
A1  - Zandanel, F.
A1  - Zanin, R.
A1  - Arlen, T.
A1  - Aune, T.
A1  - Beilicke, M.
A1  - Benbow, W.
A1  - Bouvier, A.
A1  - Bradbury, S. M.
A1  - Buckley, J. H.
A1  - Bugaev, V.
A1  - Byrum, K.
A1  - Cannon, A.
A1  - Cesarini, A.
A1  - Ciupik, L.
A1  - Connolly, M. P.
A1  - Cui, W.
A1  - Dickherber, R.
A1  - Duke, C.
A1  - Errando, M.
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A1  - Lang, M. J.
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A1  - Pohl, Martin
A1  - Prokoph, H.
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A1  - Sentuerk, G. D.
A1  - Telezhinsky, Igor O.
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A1  - Williams, D. A.
A1  - Zitzer, B.
A1  - de Almeida, U. Barres
A1  - Cara, M.
A1  - Casadio, C.
A1  - Cheung, C. C.
A1  - McConville, W.
A1  - Davies, F.
A1  - Doi, A.
A1  - Giovannini, G.
A1  - Giroletti, M.
A1  - Hada, K.
A1  - Hardee, P.
A1  - Harris, D. E.
A1  - Junor, W.
A1  - Kino, M.
A1  - Lee, N. P.
A1  - Ly, C.
A1  - Madrid, J.
A1  - Massaro, F.
A1  - Mundell, C. G.
A1  - Nagai, H.
A1  - Perlman, E. S.
A1  - Steele, I. A.
A1  - Walker, R. C.
A1  - Wood, D. L.
T1  - The 2010 very high energy gamma-ray flare and 10 years ofmulti-wavelength oservations of M 87
JF  - The astrophysical journal : an international review of spectroscopy and astronomical physics
N2  - The giant radio galaxy M 87 with its proximity (16 Mpc), famous jet, and very massive black hole ((3-6) x 10(9) M-circle dot) provides a unique opportunity to investigate the origin of very high energy (VHE; E > 100 GeV) gamma-ray emission generated in relativistic outflows and the surroundings of supermassive black holes. M 87 has been established as a VHE gamma-ray emitter since 2006. The VHE gamma-ray emission displays strong variability on timescales as short as a day. In this paper, results from a joint VHE monitoring campaign on M 87 by the MAGIC and VERITAS instruments in 2010 are reported. During the campaign, a flare at VHE was detected triggering further observations at VHE (H.E.S.S.), X-rays (Chandra), and radio (43 GHz Very Long Baseline Array, VLBA). The excellent sampling of the VHE gamma-ray light curve enables one to derive a precise temporal characterization of the flare: the single, isolated flare is well described by a two-sided exponential function with significantly different flux rise and decay times of tau(rise)(d) = (1.69 +/- 0.30) days and tau(decay)(d) = (0.611 +/- 0.080) days, respectively. While the overall variability pattern of the 2010 flare appears somewhat different from that of previous VHE flares in 2005 and 2008, they share very similar timescales (similar to day), peak fluxes (Phi(>0.35 TeV) similar or equal to (1-3) x 10(-11) photons cm(-2) s(-1)), and VHE spectra. VLBA radio observations of 43 GHz of the inner jet regions indicate no enhanced flux in 2010 in contrast to observations in 2008, where an increase of the radio flux of the innermost core regions coincided with a VHE flare. On the other hand, Chandra X-ray observations taken similar to 3 days after the peak of the VHE gamma-ray emission reveal an enhanced flux from the core (flux increased by factor similar to 2; variability timescale <2 days). The long-term (2001-2010) multi-wavelength (MWL) light curve of M 87, spanning from radio to VHE and including data from Hubble Space Telescope, Liverpool Telescope, Very Large Array, and European VLBI Network, is used to further investigate the origin of the VHE gamma-ray emission. No unique, common MWL signature of the three VHE flares has been identified. In the outer kiloparsec jet region, in particular in HST-1, no enhanced MWL activity was detected in 2008 and 2010, disfavoring it as the origin of the VHE flares during these years. Shortly after two of the three flares (2008 and 2010), the X-ray core was observed to be at a higher flux level than its characteristic range (determined from more than 60 monitoring observations: 2002-2009). In 2005, the strong flux dominance of HST-1 could have suppressed the detection of such a feature. Published models for VHE gamma-ray emission from M 87 are reviewed in the light of the new data.
KW  - galaxies: active
KW  - galaxies: individual (M 87)
KW  - galaxies: jets
KW  - galaxies: nuclei
KW  - gamma rays: galaxies
KW  - radiation mechanisms: non-thermal
Y1  - 2012
U6  - https://doi.org/10.1088/0004-637X/746/2/151
SN  - 0004-637X
VL  - 746
IS  - 2
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  - 
TY  - JOUR
A1  - Ahnen, M. L.
A1  - Ansoldi, S.
A1  - Antonelli, L. A.
A1  - Arcaro, C.
A1  - Babie, A.
A1  - Banerjee, B.
A1  - Bangale, P.
A1  - de Almeida, U. Barres
A1  - Barrio, J. A.
A1  - Gonzalez, J. Becerra
A1  - Bednarek, W.
A1  - Bernardini, E.
A1  - Berti, A.
A1  - Biasuzzi, B.
A1  - Biland, A.
A1  - Blanch, O.
A1  - Bonnefoy, S.
A1  - Bonnoli, G.
A1  - Borracci, F.
A1  - Carosi, R.
A1  - Carosi, A.
A1  - Chatterjee, A.
A1  - Colin, P.
A1  - Colombo, E.
A1  - Contreras, J. L.
A1  - Cortina, J.
A1  - Covino, S.
A1  - Cumani, P.
A1  - Da Vela, P.
A1  - Dazzi, F.
A1  - De Angelis, A.
A1  - De Lotto, B.
A1  - Wilhelmi, E. de Ona
A1  - Di Pierro, F.
A1  - Doert, M.
A1  - Dominguez, A.
A1  - Prester, D. Dominis
A1  - Dorner, D.
A1  - Doro, M.
A1  - Einecke, S.
A1  - Glawion, D. Eisenacher
A1  - Elsaesser, D.
A1  - Engelkemeier, M.
A1  - Ramazani, V. Fallah
A1  - Fernandez-Barra, A.
A1  - Fidalgo, D.
A1  - Fonseca, M. V.
A1  - Font, L.
A1  - Fruck, C.
A1  - Galindo, D.
A1  - Lopez, R. J. Garcia
A1  - Garczarczyk, M.
A1  - Gaug, M.
A1  - Giammaria, P.
A1  - Godinovie, N.
A1  - Gora, D.
A1  - Griffiths, S.
A1  - Guberman, D.
A1  - Hadasch, D.
A1  - Hahn, A.
A1  - Hassan, T.
A1  - Hayashida, M.
A1  - Herrera, J.
A1  - Hose, J.
A1  - Hrupec, D.
A1  - Hughes, G.
A1  - Ishio, K.
A1  - Konno, Y.
A1  - Kubo, H.
A1  - Kushida, J.
A1  - Kuvezdie, D.
A1  - Lelas, D.
A1  - Lindfors, E.
A1  - Lombardi, S.
A1  - Longo, F.
A1  - Lopez, M.
A1  - Lopez-Oramas, A.
A1  - Majumdar, P.
A1  - Makariev, M.
A1  - Maneva, G.
A1  - Manganaro, M.
A1  - Mannheim, K.
A1  - Maraschi, L.
A1  - Mariotti, M.
A1  - Martinez, M.
A1  - Mazin, D.
A1  - Menzel, U.
A1  - Minev, M.
A1  - Mirzoyan, R.
A1  - Moralejo, A.
A1  - Moreno, V.
A1  - Moretti, E.
A1  - Munar-Adrover, P.
A1  - Neustroev, V.
A1  - Niedzwiecki, A.
A1  - Rosillo, M. Nievas
A1  - Nilsson, K.
A1  - Nishijima, K.
A1  - Noda, K.
A1  - Nogues, L.
A1  - Paiano, S.
A1  - Palacio, J.
A1  - Paneque, D.
A1  - Paoletti, R.
A1  - Paredes, J. M.
A1  - Paredes-Fortuny, X.
A1  - Pedaletti, G.
A1  - Peresano, M.
A1  - Perri, L.
A1  - Persic, M.
A1  - Moroni, P. G. Prada
A1  - Prandini, E.
A1  - Puljak, I.
A1  - Garcia, J. R.
A1  - Reichardt, I.
A1  - Rhode, W.
A1  - Riti, M.
A1  - Rico, J.
A1  - Saito, T.
A1  - Satalecka, K.
A1  - Schroeder, S.
A1  - Schweizer, T.
A1  - Shore, S. N.
A1  - Sillanpaa, A.
A1  - Sitarek, J.
A1  - Sobczynskall, D.
A1  - Stamerra, A.
A1  - Strzys, M.
A1  - Surie, T.
A1  - Takalo, L.
A1  - Tavecchio, F.
A1  - Temnikov, P.
A1  - Terzie, T.
A1  - Tescaro, D.
A1  - Teshima, M.
A1  - Torres, D. F.
A1  - Torres-Alla, N.
A1  - Treves, A.
A1  - Vanzo, G.
A1  - Acosta, M. Vazquez
A1  - Vovk, I.
A1  - Ward, J. E.
A1  - Will, M.
A1  - Wu, M. H.
A1  - Zarie, D.
A1  - Abdalla, Hassan E.
A1  - Abramowski, A.
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A1  - Carr, J.
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A1  - Cerruti, M.
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A1  - Gottschal, D.
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A1  - Grondin, M. -H.
A1  - Hahn, J.
A1  - Haupt, M.
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A1  - Katsuragawa, M.
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A1  - Murach, T.
A1  - Nakashima, S.
A1  - De Naurois, M.
A1  - Niederwanger, F.
A1  - Niemiec, J.
A1  - Oakes, L.
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A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Padovani, M.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Pekeur, N. W.
A1  - Pelletier, G.
A1  - Perennes, C.
A1  - Petrucci, P. -O.
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A1  - Pie, Q.
A1  - Pita, S.
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A1  - Santangelo, Andrea
A1  - Sasaki, M.
A1  - Schlickeiser, R.
A1  - Schtissler, F.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwemmer, S.
A1  - Seglar-Arroyo, M.
A1  - Settimo, M.
A1  - Seyffert, A. S.
A1  - Shafi, N.
A1  - Shilon, I.
A1  - Simoni, R.
A1  - So, H.
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A1  - Spengler, G.
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A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Stycz, K.
A1  - Sushch, I.
A1  - Takahashi, T.
A1  - Tavernet, J. -P.
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tibaldo, L.
A1  - Tiziani, D.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Tsuji, N.
A1  - Tuffs, R.
A1  - Uchiyama, Y.
A1  - Van der Walt, D. J.
A1  - Van Eldik, C.
A1  - Van Rensburg, C.
A1  - Van Soelen, B.
A1  - Vasileiadis, G.
A1  - Veh, J.
A1  - Venter, C.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voisin, F.
A1  - Vok, H. J.
A1  - Vuillaume, T.
A1  - Wadiasingh, Z.
A1  - Wagner, S. J.
A1  - Wagner, P.
A1  - Wagner, R. M.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Willmann, P.
A1  - Wornlein, A.
A1  - Wouters, D.
A1  - Yang, R.
A1  - Zabalza, V.
A1  - Zaborov, D.
A1  - Zacharias, M.
A1  - Zanin, R.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zefi, F.
A1  - Ziegler, A.
A1  - Zywuckan, N.
T1  - Constraints on particle acceleration in SS433/W50 from MAGIC and HESS observations
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. The large jet kinetic power and non-thermal processes occurring in the microquasar SS 433 make this source a good candidate for a very high-energy (VHE) gamma-ray emitter. Gamma-ray fluxes above the sensitivity limits of current Cherenkov telescopes have been predicted for both the central X-ray binary system and the interaction regions of SS 433 jets with the surrounding W50 nebula. Non-thermal emission at lower energies has been previously reported, indicating that efficient particle acceleration is taking place in the system. Aims. We explore the capability of SS 433 to emit VHE gamma rays during periods in which the expected flux attenuation due to periodic eclipses (P-orb similar to 13.1 days) and precession of the circumstellar disk (P-pre similar to 162 days) periodically covering the central binary system is expected to be at its minimum. The eastern and western SS 433/W50 interaction regions are also examined using the whole data set available. We aim to constrain some theoretical models previously developed for this system with our observations. Methods. We made use of dedicated observations from the Major Atmospheric Gamma Imaging Cherenkov telescopes (MAGIC) and High Energy Spectroscopic System (H.E.S.S.) of SS 433 taken from 2006 to 2011. These observation were combined for the first time and accounted for a total effective observation time of 16.5 h, which were scheduled considering the expected phases of minimum absorption of the putative VHE emission. Gamma-ray attenuation does not affect the jet/medium interaction regions. In this case, the analysis of a larger data set amounting to similar to 40-80 h, depending on the region, was employed. Results. No evidence of VHE gamma-ray emission either from the central binary system or from the eastern/western interaction regions was found. Upper limits were computed for the combined data set. Differential fluxes from the central system are found to be less than or similar to 10(-12)-10(-13) TeV-1 cm(-2) s(-1) in an energy interval ranging from similar to few x 100 GeV to similar to few TeV. Integral flux limits down to similar to 10(-12)-10(-13) ph cm(-2) s(-1) and similar to 10(-13)-10(-14) ph cm(-2) s(-1) are obtained at 300 and 800 GeV, respectively. Our results are used to place constraints on the particle acceleration fraction at the inner jet regions and on the physics of the jet/medium interactions. Conclusions. Our findings suggest that the fraction of the jet kinetic power that is transferred to relativistic protons must be relatively small in SS 433, q(p) <= 2.5 x 10(-5), to explain the lack of TeV and neutrino emission from the central system. At the SS 433/W50 interface, the presence of magnetic fields greater than or similar to 10 mu G is derived assuming a synchrotron origin for the observed X-ray emission. This also implies the presence of high-energy electrons with E-e up to 50 TeV, preventing an efficient production of gamma-ray fluxes in these interaction regions.
KW  - gamma rays: general
KW  - stars: black holes
KW  - X-rays: binaries
KW  - ISM: jets and outflows
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201731169
SN  - 1432-0746
VL  - 612
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Abdalla, Hassan E.
A1  - Adam, R.
A1  - Aharonian, Felix A.
A1  - Benkhali, F. Ait
A1  - Angüner, Ekrem Oǧuzhan
A1  - Arakawa, M.
A1  - Arcaro, C.
A1  - Armand, C.
A1  - Ashkar, H.
A1  - Backes, M.
A1  - Martins, V. Barbosa
A1  - Barnard, M.
A1  - Becherini, Y.
A1  - Berge, D.
A1  - Bernloehr, K.
A1  - Blackwell, R.
A1  - Böttcher, M.
A1  - Boisson, C.
A1  - Bolmont, J.
A1  - Bonnefoy, S.
A1  - Bregeon, J.
A1  - Breuhaus, M.
A1  - Brun, F.
A1  - Brun, P.
A1  - Bryan, M.
A1  - Büchele, M.
A1  - Bulik, T.
A1  - Bylund, T.
A1  - Capasso, M.
A1  - Caroff, S.
A1  - Carosi, A.
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chand, T.
A1  - Chandra, S.
A1  - Chen, A.
A1  - Colafrancesco, S.
A1  - Curylo, M.
A1  - Davids, I. D.
A1  - Deil, C.
A1  - Devin, J.
A1  - DeWilt, P.
A1  - Dirson, L.
A1  - Djannati-Ata, A.
A1  - Dmytriiev, A.
A1  - Donath, A.
A1  - Doroshenko, V
A1  - Dyks, J.
A1  - Egberts, Kathrin
A1  - Emery, G.
A1  - Ernenwein, J-P
A1  - Eschbach, S.
A1  - Feijen, K.
A1  - Fegan, S.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Funk, S.
A1  - Füßling, Matthias
A1  - Gabici, S.
A1  - Gallant, Y. A.
A1  - Gate, F.
A1  - Giavitto, G.
A1  - Glawion, D.
A1  - Glicenstein, J. F.
A1  - Gottschall, D.
A1  - Grondin, M-H
A1  - Hahn, J.
A1  - Haupt, M.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hinton, James Anthony
A1  - Hofmann, W.
A1  - Hoischen, Clemens
A1  - Holch, Tim Lukas
A1  - Holler, M.
A1  - Horns, D.
A1  - Huber, D.
A1  - Iwasaki, H.
A1  - Jamrozy, M.
A1  - Jankowsky, D.
A1  - Jankowsky, F.
A1  - Jardin-Blicq, A.
A1  - Jung-Richardt, I
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katsuragawa, M.
A1  - Katz, U.
A1  - Khangulyan, D.
A1  - Khelifi, B.
A1  - King, J.
A1  - Klepser, S.
A1  - Kluzniak, W.
A1  - Komin, Nu
A1  - Kosack, K.
A1  - Kostunin, D.
A1  - Kraus, M.
A1  - Lamanna, G.
A1  - Lau, J.
A1  - Lemiere, A.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J-P
A1  - Leser, Eva
A1  - Levy, C.
A1  - Lohse, T.
A1  - Lypova, I
A1  - Mackey, J.
A1  - Majumdar, J.
A1  - Malyshev, D.
A1  - Marandon, V
A1  - Marcowith, Alexandre
A1  - Mares, A.
A1  - Mariaud, C.
A1  - Marti-Devesa, G.
A1  - Marx, R.
A1  - Maurin, G.
A1  - Meintjes, P. J.
A1  - Mitchell, A. M. W.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Mohrmann, L.
A1  - Moore, C.
A1  - Moulin, Emmanuel
A1  - Muller, J.
A1  - Murach, T.
A1  - Nakashima, S.
A1  - de Naurois, M.
A1  - Ndiyavala, H.
A1  - Niederwanger, F.
A1  - Niemiec, J.
A1  - Oakes, L.
A1  - Odaka, H.
A1  - Ohm, S.
A1  - Wilhelmi, E. de Ona
A1  - Ostrowski, M.
A1  - Oya, I
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Perennes, C.
A1  - Petrucci, P-O
A1  - Peyaud, B.
A1  - Piel, Q.
A1  - Pita, S.
A1  - Poireau, V
A1  - Priyana Noel, A.
A1  - Prokhorov, D. A.
A1  - Prokoph, H.
A1  - Pühlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Rauth, R.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Remy, Q.
A1  - Renaud, M.
A1  - Rieger, F.
A1  - Rinchiuso, L.
A1  - Romoli, C.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Ruiz-Velasco, E.
A1  - Sahakian, V
A1  - Saito, S.
A1  - Sanchez, David M.
A1  - Santangelo, Andrea
A1  - Sasaki, M.
A1  - Schlickeiser, R.
A1  - Schüssler, F.
A1  - Schulz, A.
A1  - Schutte, H.
A1  - Schwanke, U.
A1  - Schwemmer, S.
A1  - Seglar-Arroyo, M.
A1  - Senniappan, M.
A1  - Seyffert, A. S.
A1  - Shafi, N.
A1  - Shiningayamwe, K.
A1  - Simoni, R.
A1  - Sinha, A.
A1  - Sol, H.
A1  - Specovius, A.
A1  - Spir-Jacob, M.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Steppa, Constantin Beverly
A1  - Takahashi, T.
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tiziani, D.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Tsirou, M.
A1  - Tsuji, N.
A1  - Tuffs, R.
A1  - Uchiyama, Y.
A1  - van Der Walt, D. J.
A1  - van Eldik, C.
A1  - van Rensburg, C.
A1  - van Soelen, B.
A1  - Vasileiadis, G.
A1  - Veh, J.
A1  - Venter, C.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voisin, F.
A1  - Voelk, H. J.
A1  - Vuillaume, T.
A1  - Wadiasingh, Z.
A1  - Wagner, S. J.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Yang, R.
A1  - Yoneda, H.
A1  - Zacharias, Michael
A1  - Zanin, R.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Ziegler, A.
A1  - Zorn, J.
A1  - Zywucka, N.
A1  - Meyer, M.
T1  - Constraints on the emission region of 3C 279 during strong flares in 2014 and 2015 through VHE gamma-ray observations with HESS
JF  - Astronomy and astrophysics : an international weekly journal
N2  - The flat spectrum radio quasar 3C 279 is known to exhibit pronounced variability in the high-energy (100MeV < E < 100 GeV) gamma-ray band, which is continuously monitored with Fermi-LAT. During two periods of high activity in April 2014 and June 2015 target-of-opportunity observations were undertaken with the High Energy Stereoscopic System (H.E.S.S.) in the very-high-energy (VHE, E > 100 GeV) gamma-ray domain. While the observation in 2014 provides an upper limit, the observation in 2015 results in a signal with 8 : 7 sigma significance above an energy threshold of 66 GeV. No VHE variability was detected during the 2015 observations. The VHE photon spectrum is soft and described by a power-law index of 4.2 +/- 0.3. The H.E.S.S. data along with a detailed and contemporaneous multiwavelength data set provide constraints on the physical parameters of the emission region. The minimum distance of the emission region from the central black hole was estimated using two plausible geometries of the broad-line region and three potential intrinsic spectra. The emission region is confidently placed at r greater than or similar to 1 : 7 X 1017 cm from the black hole, that is beyond the assumed distance of the broad-line region. Time-dependent leptonic and lepto-hadronic one-zone models were used to describe the evolution of the 2015 flare. Neither model can fully reproduce the observations, despite testing various parameter sets. Furthermore, the H.E.S.S. data were used to derive constraints on Lorentz invariance violation given the large redshift of 3C 279.
KW  - radiation mechanisms: non-thermal
KW  - quasars: individual: 3C 279
KW  - galaxies: active
KW  - relativistic processes
Y1  - 2019
U6  - https://doi.org/10.1051/0004-6361/201935704
SN  - 1432-0746
VL  - 627
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Abdalla, Hassan E.
A1  - Collaboration, H. E. S. S.
A1  - Abramowski, A.
A1  - Aharonian, Felix A.
A1  - Benkhali, F. Ait
A1  - Angüner, Ekrem Oǧuzhan
A1  - Arakawa, M.
A1  - Armand, C.
A1  - Arrieta, M.
A1  - Backes, M.
A1  - Balzer, A.
A1  - Barnard, M.
A1  - Becherini, Y.
A1  - Tjus, J. Becker
A1  - Berge, D.
A1  - Bernhard, S.
A1  - Bernloehr, K.
A1  - Blackwell, R.
A1  - Bottcher, M.
A1  - Boisson, C.
A1  - Bolmont, J.
A1  - Bonnefoy, S.
A1  - Bordas, Pol
A1  - Bregeon, J.
A1  - Brun, F.
A1  - Brun, P.
A1  - Bryan, M.
A1  - Buechele, M.
A1  - Bulik, T.
A1  - Capasso, M.
A1  - Caroff, S.
A1  - Carosi, A.
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chakraborty, N.
A1  - Chaves, R. C. G.
A1  - Chen, A.
A1  - Chevalier, J.
A1  - Colafrancesco, S.
A1  - Condon, B.
A1  - Conrad, J.
A1  - Davids, I. D.
A1  - Decock, J.
A1  - Deil, C.
A1  - Devin, J.
A1  - deWilt, P.
A1  - Dirson, L.
A1  - Djannati-Atai, A.
A1  - Donath, A.
A1  - Dyks, J.
A1  - Edwards, T.
A1  - Egberts, Kathrin
A1  - Emery, G.
A1  - Ernenwein, J. -P.
A1  - Eschbach, S.
A1  - Farnier, C.
A1  - Fegan, S.
A1  - Fernandes, M. V.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Funk, S.
A1  - Fuessling, M.
A1  - Gabici, S.
A1  - Gallant, Y. A.
A1  - Garrigoux, T.
A1  - Gate, F.
A1  - Giavitto, G.
A1  - Glawion, D.
A1  - Glicenstein, J. F.
A1  - Gottschall, D.
A1  - Grondin, M. -H.
A1  - Hahn, J.
A1  - Haupt, M.
A1  - Hawkes, J.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hinton, J. A.
A1  - Hofmann, W.
A1  - Hoischen, Clemens
A1  - Holch, T. L.
A1  - Holler, M.
A1  - Horns, D.
A1  - Ivascenko, A.
A1  - Iwasaki, H.
A1  - Jacholkowska, A.
A1  - Jamrozy, M.
A1  - Jankowsky, D.
A1  - Jankowsky, F.
A1  - Jingo, M.
A1  - Jouvin, L.
A1  - Jung-Richardt, I.
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katsuragawa, M.
A1  - Katz, U.
A1  - Kerszberg, D.
A1  - Khangulyan, D.
A1  - Khelifi, B.
A1  - King, J.
A1  - Klepser, S.
A1  - Klochkov, D.
A1  - Kluzniak, W.
A1  - Komin, Nu.
A1  - Kosack, K.
A1  - Krakau, S.
A1  - Kraus, M.
A1  - Kruger, P. P.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lau, J.
A1  - Lefaucheur, J.
A1  - Lemiere, A.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J. -P.
A1  - Leser, Eva
A1  - Lohse, T.
A1  - Lorentz, M.
A1  - Liu, R.
A1  - Lopez-Coto, R.
A1  - Lypova, I.
A1  - Malyshev, D.
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Mariaud, C.
A1  - Marx, R.
A1  - Maurin, G.
A1  - Maxted, N.
A1  - Mayer, M.
A1  - Meintjes, P. J.
A1  - Meyer, M.
A1  - Mitchell, A. M. W.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Mohrmann, L.
A1  - Mora, K.
A1  - Moulin, Emmanuel
A1  - Murach, T.
A1  - Nakashima, S.
A1  - de Naurois, M.
A1  - Ndiyavala, H.
A1  - Niederwanger, F.
A1  - Niemiec, J.
A1  - Oakes, L.
A1  - Odaka, H.
A1  - Ohm, S.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Padovani, M.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Pekeur, N. W.
A1  - Pelletier, G.
A1  - Perennes, C.
A1  - Petrucci, P. -O.
A1  - Peyaud, B.
A1  - Piel, Q.
A1  - Pita, S.
A1  - Poireau, V.
A1  - Prokhorov, D. A.
A1  - Prokoph, H.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Rauth, R.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - de los Reyes, R.
A1  - Rieger, F.
A1  - Rinchiuso, L.
A1  - Romoli, C.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Sahakian, V.
A1  - Saito, S.
A1  - Sanchez, D. A.
A1  - Santangelo, Andrea
A1  - Sasaki, M.
A1  - Schlickeiser, R.
A1  - Schussler, F.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwemmer, S.
A1  - Seglar-Arroyo, M.
A1  - Seyffert, A. S.
A1  - Shafi, N.
A1  - Shilon, I.
A1  - Shiningayamwe, K.
A1  - Simoni, R.
A1  - Sol, H.
A1  - Spanier, F.
A1  - Spir-Jacob, M.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Steppa, Constantin Beverly
A1  - Sushch, I.
A1  - Takahashi, T.
A1  - Tavernet, J. -P.
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tibaldo, L.
A1  - Tiziani, D.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Tsirou, M.
A1  - Tsuji, N.
A1  - Tuffs, R.
A1  - Uchiyama, Y.
A1  - van der Walt, D. J.
A1  - van Eldik, C.
A1  - van Rensburg, C.
A1  - van Soelen, B.
A1  - Vasileiadis, G.
A1  - Veh, J.
A1  - Venter, C.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voisin, F.
A1  - Voelk, H. J.
A1  - Vuillaume, T.
A1  - Wadiasingh, Z.
A1  - Wagner, S. J.
A1  - Wagner, P.
A1  - Wagner, R. M.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Willmann, P.
A1  - Woernlein, A.
A1  - Wouters, D.
A1  - Yang, R.
A1  - Zaborov, D.
A1  - Zacharias, M.
A1  - Zanin, R.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zefi, F.
A1  - Ziegler, A.
A1  - Zorn, J.
A1  - Zywucka, N.
T1  - Detection of variable VHE gamma-ray emission from the extra-galactic gamma-ray binary LMC P3
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. Recently, the high-energy (HE, 0.1-100 GeV) gamma-ray emission from the object LMC P3 in the Large Magellanic Cloud (LMC) has been discovered to be modulated with a 10.3-day period, making it the first extra-galactic gamma-ray binary. Aims. This work aims at the detection of very-high-energy (VHE, >100 GeV) gamma-ray emission and the search for modulation of the VHE signal with the orbital period of the binary system. Methods. LMC P3 has been observed with the High Energy Stereoscopic System (H.E.S.S.); the acceptance-corrected exposure time is 100 h. The data set has been folded with the known orbital period of the system in order to test for variability of the emission. Results. VHE gamma-ray emission is detected with a statistical significance of 6.4 sigma. The data clearly show variability which is phase-locked to the orbital period of the system. Periodicity cannot be deduced from the H.E.S.S. data set alone. The orbit-averaged luminosity in the 1-10 TeV energy range is (1.4 +/- 0.2) x 10(35) erg s(-1). A luminosity of (5 +/- 1) x 10(35) erg s(-1) is reached during 20% of the orbit. HE and VHE gamma-ray emissions are anti-correlated. LMC P3 is the most luminous gamma-ray binary known so far.
KW  - gamma rays: stars
KW  - binaries: general
KW  - stars: massive
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201732426
SN  - 1432-0746
VL  - 610
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Abramowski, Attila
A1  - Aharonian, Felix A.
A1  - Benkhali, Faical  Ait
A1  - Akhperjanian, A. G.
A1  - Angüner, Ekrem Oǧuzhan
A1  - Backes, Michael
A1  - Balenderan, Shangkari
A1  - Balzer, Arnim
A1  - Barnacka, Anna
A1  - Becherini, Yvonne
A1  - Tjus, J. Becker
A1  - Berge, David
A1  - Bernhard, Sabrina
A1  - Bernlöhr, K.
A1  - Birsin, E.
A1  - Biteau, Jonathan
A1  - Boettcher, Markus
A1  - Boisson, Catherine
A1  - Bolmont, J.
A1  - Bordas, Pol
A1  - Bregeon, Johan
A1  - Brun, Francois
A1  - Brun, Pierre
A1  - Bryan, Mark
A1  - Bulik, Tomasz
A1  - Carrigan, Svenja
A1  - Casanova, Sabrina
A1  - Chadwick, Paula M.
A1  - Chatraborty, N.
A1  - Chalme-Calvet, R.
A1  - Chaves, Ryan C. G.
A1  - Chretien, M.
A1  - Colafrancesco, Sergio
A1  - Cologna, Gabriele
A1  - Conrad, Jan
A1  - Couturier, C.
A1  - Cui, Y.
A1  - Davids, I. D.
A1  - Degrange, B.
A1  - Deil, C.
A1  - deWilt, P.
A1  - Djannati-Ataï, A.
A1  - Domainko, W.
A1  - Donath, A.
A1  - Dubus, G.
A1  - Dutson, K.
A1  - Dyks, J.
A1  - Dyrda, M.
A1  - Edwards, T.
A1  - Egberts, Kathrin
A1  - Eger, P.
A1  - Espigat, P.
A1  - Farnier, C.
A1  - Fegan, S.
A1  - Feinstein, F.
A1  - Fernandes, M. V.
A1  - Fernandez, D.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Foerster, A.
A1  - Fuessling, M.
A1  - Gabici, S.
A1  - Gajdus, M.
A1  - Gallant, Y. A.
A1  - Garrigoux, T.
A1  - Giavitto, G.
A1  - Giebels, B.
A1  - Glicenstein, J. F.
A1  - Gottschall, D.
A1  - Grondin, M. -H.
A1  - Grudzinska, M.
A1  - Hadasch, D.
A1  - Haeffner, S.
A1  - Hahn, J.
A1  - Harris, J.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hervet, O.
A1  - Hillert, A.
A1  - Hinton, James Anthony
A1  - Hofmann, W.
A1  - Hofverberg, P.
A1  - Holler, Markus
A1  - Horns, D.
A1  - Ivascenko, A.
A1  - Jacholkowska, A.
A1  - Jahn, C.
A1  - Jamrozy, M.
A1  - Janiak, M.
A1  - Jankowsky, F.
A1  - Jung-Richardt, O.
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katz, U.
A1  - Kaufmann, S.
A1  - Khelifi, B.
A1  - Kieffer, M.
A1  - Klepser, S.
A1  - Klochkov, D.
A1  - Kluzniak, W.
A1  - Kolitzus, D.
A1  - Komin, Nu
A1  - Kosack, K.
A1  - Krakau, S.
A1  - Krayzel, F.
A1  - Krueger, P. P.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lefaucheur, J.
A1  - Lefranc, V.
A1  - Lemiere, A.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J. P.
A1  - Lohse, T.
A1  - Lopatin, A.
A1  - Lu, C-C
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Marx, R.
A1  - Maurin, G.
A1  - Maxted, N.
A1  - Mayer, Markus
A1  - McComb, T. J. L.
A1  - Mehault, J.
A1  - Meintjes, P. J.
A1  - Menzler, U.
A1  - Meyer, M.
A1  - Mitchell, A. M. W.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Mora, K.
A1  - Moulin, Emmanuel
A1  - Murach, T.
A1  - de Naurois, M.
A1  - Niemiec, J.
A1  - Nolan, S. J.
A1  - Oakes, L.
A1  - Odaka, H.
A1  - Ohm, S.
A1  - Opitz, B.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Anibas, M. Paz
A1  - Pekeur, N. W.
A1  - Pelletier, G.
A1  - Petrucci, P-O
A1  - Peyaud, B.
A1  - Pita, S.
A1  - Poon, H.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Reichardt, I.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - de los Reyes, R.
A1  - Rieger, F.
A1  - Romoli, C.
A1  - Rosier-Lees, S.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Sahakian, V.
A1  - Salek, D.
A1  - Sanchez, David M.
A1  - Santangelo, Andrea
A1  - Schlickeiser, R.
A1  - Schuessler, F.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwarzburg, S.
A1  - Schwemmer, S.
A1  - Sol, H.
A1  - Spanier, F.
A1  - Spengler, G.
A1  - Spies, F.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Stinzing, F.
A1  - Stycz, K.
A1  - Sushch, Iurii
A1  - Tavernet, J-P
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Valerius, K.
A1  - van Eldik, C.
A1  - van Soelen, B.
A1  - Vasileiadis, G.
A1  - Veh, J.
A1  - Venter, C.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voelk, H. J.
A1  - Volpe, F.
A1  - Vorster, M.
A1  - Vuillaume, T.
A1  - Wagner, S. J.
A1  - Wagner, P.
A1  - Wagner, R. M.
A1  - Ward, M.
A1  - Weidinger, M.
A1  - Weitzel, Q.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Willmann, P.
A1  - Woernlein, A.
A1  - Wouters, D.
A1  - Yang, R.
A1  - Zabalza, V.
A1  - Zaborov, D.
A1  - Zacharias, M.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zechlin, H-S
T1  - HESS detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud
JF  - Astronomy and astrophysics : an international weekly journal
N2  - G349.7+0.2 is a young Galactic supernova remnant (SNR) located at the distance of 11.5 kpc and observed across the entire electromagnetic spectrum from radio to high energy (HE; 0.1 GeV < E < 100 GeV) gamma-rays. Radio and infrared observations indicate that the remnant is interacting with a molecular cloud. In this paper, the detection of very high energy (VHE, E > 100 GeV) gamma-ray emission coincident with this SNR with the High Energy Stereoscopic System (HESS.) is reported. This makes it one of the farthest Galactic SNR ever detected in this domain. An integral flux F(E > 400 GeV) = (6.5 +/- 1.1(stat) +/- 1.3(syst)) x 10-11 ph cm(-2) s(-1) corresponding to similar to 0.7% of that of the Crab Nebula and to a luminosity of similar to 10(34) erg s(-1) above the same energy threshold, and a steep photon index Gamma(VHE) = 2.8 +/- 0.27(stat) +/- 0.20(syst) are measured. The analysis of more than 5 yr of Fermi-LAT data towards this source shows a power-law like spectrum with a best-fit photon index Gamma(HE) = 2.2 +/- 0.04.2(stat-0.31sys)(+0.13), The combined gamma-ray spectrum of 0349.7+0.2 can be described by either a broken power law (I3PL) or a power law with exponential (or sub exponential) cutoff (PLC). In the former case, the photon break energy is found at E-br,E-gamma = 551(-30)(+70) GeV, slightly higher than what is usually observed in the HE/VHE gamma-ray emitting middle-aged SNRs known to be interacting with molecular clouds. In the latter case. the exponential (respectively sub-exponential) cutoff energy is measured at E-cat,E-gamma = 1.4(-0.55)(+1.6) (respectively 0.35(-0.21)(+0.75)) TeV. A pion decay process resulting from the interaction of the accelerated protons and nuclei with the dense surrounding medium is clearly the preferred scenario to explain the gamma-ray emission. The BPL with a spectral steepening of 0.5-1 and the PLC provide equally good fits to the data. The product or the average gas density and the total energy content of accelerated protons and nuclei amounts to nu W-p similar to 5 x 10(51) erg cm(-3)
KW  - gamma rays: general
KW  - ISM: supernova remnants
KW  - ISM: clouds
Y1  - 2015
U6  - https://doi.org/10.1051/0004-6361/201425070
SN  - 0004-6361
SN  - 1432-0746
VL  - 574
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - THES
A1  - Foster, Mary Grace
T1  - X-Ray studies of exoplanet systems
N2  - X-rays are integral to furthering our knowledge of exoplanetary systems. In this work we discuss the use of X-ray observations to understand star-planet interac- tions, mass-loss rates of an exoplanet’s atmosphere and the study of an exoplanet’s atmospheric components using future X-ray spectroscopy.
The low-mass star GJ 1151 was reported to display variable low-frequency radio emission, which is an indication of coronal star-planet interactions with an unseen exoplanet. In chapter 5 we report the first X-ray detection of GJ 1151’s corona based on XMM-Newton data. Averaged over the observation, we detect the star with a low coronal temperature of 1.6 MK and an X-ray luminosity of LX = 5.5 × 1026 erg/s. This is compatible with the coronal assumptions for a sub-Alfvénic star- planet interaction origin of the observed radio signals from this star.
In chapter 6, we aim to characterise the high-energy environment of known ex- oplanets and estimate their mass-loss rates. This work is based on the soft X-ray instrument on board the Spectrum Roentgen Gamma (SRG) mission, eROSITA, along with archival data from ROSAT, XMM-Newton, and Chandra. We use these four X-ray source catalogues to derive X-ray luminosities of exoplanet host stars in the 0.2-2 keV energy band. A catalogue of the mass-loss rates of 287 exoplan- ets is presented, with 96 of these planets characterised for the first time using new eROSITA detections. Of these first time detections, 14 are of transiting exoplanets that undergo irradiation from their host stars that is of a level known to cause ob- servable evaporation signals in other systems, making them suitable for follow-up observations.
In the next generation of space observatories, X-ray transmission spectroscopy of an exoplanet’s atmosphere will be possible, allowing for a detailed look into the atmospheric composition of these planets. In chapter 7, we model sample spectra using a toy model of an exoplanetary atmosphere to predict what exoplanet transit observations with future X-ray missions such as Athena will look like. We then estimate the observable X-ray transmission spectrum for a typical Hot Jupiter-type exoplanet, giving us insights into the advances in X-ray observations of exoplanets in the decades to come.
N2  - Röntgenstrahlen sind ein wesentlicher Bestandteil, um unser Wissen über extrasolare Planetensysteme zu vertiefen und zu erweitern. In dieser Arbeit erörtern wir den Einsatz von Röntgenbeobachtungen zum Verständnis von Stern-Planeten-Interaktionen, der Abschätzung von Massenverlustraten von Exoplanetenatmosphären und die Untersuchung der atmosphärischen Komponenten eines Exoplaneten mithilfe zukünftiger Röntgenspektroskopie.

Beobachtungen des massearmen Sterns GJ 1151 deuten auf eine variable Emission niederfrequenter Radiostrahlung hin, was als Indiz für koronale Stern-Planeten-Wechselwirkungen mit einem unsichtbaren Exoplaneten angesehen wird. In Kapitel 5 berichten wir über den ersten Röntgennachweis der Korona von GJ 1151, basierend auf XMM-Newton Daten. Über die gesamte Beobachtungsdauer gemittelt, weisen wir den Stern mit einer niedrigen koronalen Temperatur von 1,6 MK und einer Röntgenluminosität von LX = 5, 5 ◊ 1026 erg/s nach. Dieser Nachweis im Röntgenlicht ist kompatibel mit der Annahme, dass sub-Alfvénische Wechselwirkungen zwischen stellarer Corona und Exoplanet die Ursache für die beobachteten Radiosignale des Sterns sind.

Kapitel 6 zielt darauf ab, die hochenergetische Umgebung bekannter Exoplaneten zu charakterisieren und die Massenverlustraten der Planetenatmosphären abzuschätzen. Diese Arbeit basiert auf neu gewonnenen Daten des Instruments für weiche Röntgenstrahlung an Bord der Spectrum Roentgen Gamma (SRG) Mission, eROSITA, und wird komplementiert von Archivdaten von ROSAT, XMM-Newton und Chandra. Mithilfe dieser vier Röntgenquellenkataloge vermessen wir die Röntgenhelligkeit der Zentralsterne von bekannten Exoplanetensytemen im Energiebereich von 0,2-2 keV. Die Ergebnisse sind zusammen mit den errechneten Massenverlustraten von 287 Exoplaneten in einem Katalog zusammengefasst, darunter 96 Planeten, die zum ersten Mal durch neue eROSITA-Nachweise charakterisiert wurden. Bei 14 dieser Erstnachweise handelt es sich um transitierende Exoplaneten, die von ihrem Heimatstern so stark bestrahlt werden, dass beobachtbare Signale, ausgelöst durch die Verdampfung ihrer Atmosphäre, zu erwarten sind. Speziell diese Systeme eignen sich besonders für Folgebeobachtungen.

Mit der nächsten Generation von Weltraumobservatorien wird die Röntgentransmissionsspektroskopie von extrasolaren Planetenatmosphären möglich sein, was nie dagewesene Details über die atmosphärische Zusammensetzung dieser Planeten ans Licht bringen wird. In Kapitel 7 modellieren wir Transmissionsspektren mithilfe eines vereinfachten Modells einer Exoplanetenatmosphäre um vorherzusagen, wie Transitbeobachtungen von Exoplaneten mit zukünftigen Röntgenmissionen wie Athena aussehen werden. Wir schätzen dann das beobachtbare Röntgentransmissionsspektrum für einen typischen Exoplaneten vom Typ Hot Jupiter ab, was uns einen Einblick in die zu erwartenden Fortschritte bei der Röntgenbeobachtung von Exoplaneten in den kommenden Jahrzehnten gibt.
KW  - exoplanets
KW  - x-rays
KW  - stellar physics
KW  - Exoplaneten
KW  - Röntgenstrahlen
KW  - stellare Physik
Y1  - 2022
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-562152
PB  - xiii, 92
ER  - 
TY  - JOUR
A1  - Schwope, Axel
A1  - Pires, Adriana M.
A1  - Kurpas, Jan
A1  - Doroshenko, Victor
A1  - Suleimanov, Valery F.
A1  - Freyberg, Michael
A1  - Becker, Werner
A1  - Dennerl, Konrad
A1  - Haberl, Frank
A1  - Lamer, Georg
A1  - Maitra, Chandreyee
A1  - Potekhin, Alexander Y.
A1  - Ramos-Ceja, Miriam E.
A1  - Santangelo, Andrea
A1  - Traulsen, Iris
A1  - Werner, Klaus
T1  - Phase-resolved X-ray spectroscopy of PSR B0656+14 with SRG/eROSITA and XMM-Newton
JF  - Astronomy and astrophysics : an international weekly journal
N2  - We present a detailed spectroscopic and timing analysis of X-ray observations of the bright pulsar PSR B0656+14. The observations were obtained simultaneously with eROSITA and XMM-Newton during the calibration and performance verification phase of the Spektrum-Roentgen-Gamma mission (SRG). The analysis of the 100 ks deep observation of eROSITA is supported by archival observations of the source, including XMM-Newton, NuSTAR, and NICER. Using XMM-Newton and NICER, we first established an X-ray ephemeris for the time interval 2015 to 2020, which connects all X-ray observations in this period without cycle count alias and phase shifts. The mean eROSITA spectrum clearly reveals an absorption feature originating from the star at 570 eV with a Gaussian sigma of about 70 eV that was tentatively identified in a previous long XMM-Newton observation. A second previously discussed absorption feature occurs at 260-265 eV and is described here as an absorption edge. It could be of atmospheric or of instrumental origin. These absorption features are superposed on various emission components that are phenomenologically described here as the sum of hot (120 eV) and cold (65 eV) blackbody components, both of photospheric origin, and a power law with photon index Gamma = 2 from the magnetosphere. We created energy-dependent light curves and phase-resolved spectra with a high signal-to-noise ratio. The phase-resolved spectroscopy reveals that the Gaussian absorption line at 570 eV is clearly present throughout similar to 60% of the spin cycle, but it is otherwise undetected. Likewise, its parameters were found to be dependent on phase. The visibility of the line strength coincides in phase with the maximum flux of the hot blackbody. If the line originates from the stellar surface, it nevertheless likely originates from a different location than the hot polar cap. We also present three families of model atmospheres: a magnetized atmosphere, a condensed surface, and a mixed model. They were applied to the mean observed spectrum, whose continuum fit the observed data well. The atmosphere model, however, predicts distances that are too short. For the mixed model, the Gaussian absorption may be interpreted as proton cyclotron absorption in a field as high as 10(14) G, which is significantly higher than the field derived from the moderate observed spin-down.
KW  - stars: neutron
KW  - X-rays: stars
KW  - pulsars: individual: PSR B0656+14
Y1  - 2022
U6  - https://doi.org/10.1051/0004-6361/202141105
SN  - 0004-6361
SN  - 1432-0746
VL  - 661
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Foster, Mary Grace
A1  - Poppenhäger, Katja
A1  - Ilić Petković, Nikoleta
A1  - Schwope, Axel
T1  - Exoplanet X-ray irradiation and evaporation rates with eROSITA
JF  - Astronomy and astrophysics : an international weekly journal
N2  - High-energy irradiation is a driver for atmospheric evaporation and mass loss in exoplanets. This work is based on data from eROSITA, the soft X-ray instrument on board the Spectrum Roentgen Gamma mission, as well as on archival data from other missions. We aim to characterise the high-energy environment of known exoplanets and estimate their mass-loss rates. We use X-ray source catalogues from eROSITA, XMM-Newton, Chandra, and ROSAT to derive X-ray luminosities of exoplanet host stars in the 0.2–2 keV energy band with an underlying coronal, that is, optically thin thermal spectrum. We present a catalogue of stellar X-ray and EUV luminosities, exoplanetary X-ray and EUV irradiation fluxes, and estimated mass-loss rates for a total of 287 exoplanets, 96 of which are characterised for the first time based on new eROSITA detections. We identify 14 first-time X-ray detections of transiting exoplanets that are subject to irradiation levels known to cause observable evaporation signatures in other exoplanets. This makes them suitable targets for follow-up observations.
KW  - stars: coronae
KW  - stars: activity
KW  - planet-star interactions
KW  - planets and
KW  - satellites: atmospheres
KW  - X-rays: stars
Y1  - 2022
U6  - https://doi.org/10.1051/0004-6361/202141097
SN  - 0004-6361
SN  - 1432-0746
VL  - 661
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Ye, Fangyuan
A1  - Zhang, Shuo
A1  - Warby, Jonathan
A1  - Wu, Jiawei
A1  - Gutierrez-Partida, Emilio
A1  - Lang, Felix
A1  - Shah, Sahil
A1  - Saglamkaya, Elifnaz
A1  - Sun, Bowen
A1  - Zu, Fengshuo
A1  - Shoai, Safa
A1  - Wang, Haifeng
A1  - Stiller, Burkhard
A1  - Neher, Dieter
A1  - Zhu, Wei-Hong
A1  - Stolterfoht, Martin
A1  - Wu, Yongzhen
T1  - Overcoming C₆₀-induced interfacial recombination in inverted perovskite solar cells by electron-transporting carborane
JF  - Nature Communications
N2  - Inverted perovskite solar cells still suffer from significant non-radiative recombination losses at the perovskite surface and across the perovskite/C₆₀ interface, limiting the future development of perovskite-based single- and multi-junction photovoltaics. Therefore, more effective inter- or transport layers are urgently required. To tackle these recombination losses, we introduce ortho-carborane as an interlayer material that has a spherical molecular structure and a three-dimensional aromaticity. Based on a variety of experimental techniques, we show that ortho-carborane decorated with phenylamino groups effectively passivates the perovskite surface and essentially eliminates the non-radiative recombination loss across the perovskite/C₆₀ interface with high thermal stability. We further demonstrate the potential of carborane as an electron transport material, facilitating electron extraction while blocking holes from the interface. The resulting inverted perovskite solar cells deliver a power conversion efficiency of over 23% with a low non-radiative voltage loss of 110 mV, and retain >97% of the initial efficiency after 400 h of maximum power point tracking. Overall, the designed carborane based interlayer simultaneously enables passivation, electron-transport and hole-blocking and paves the way toward more efficient and stable perovskite solar cells.
Y1  - 2022
U6  - https://doi.org/10.1038/s41467-022-34203-x
SN  - 2041-1723
VL  - 13
IS  - 1
PB  - Springer Nature
CY  - London
ER  - 
TY  - JOUR
A1  - Omel'chenko, Oleh
A1  - Ocampo-Espindola, Jorge Luis
A1  - Kiss, István Z.
T1  - Asymmetry-induced isolated fully synchronized state in coupled oscillator populations
JF  - Physical review : E, Statistical, nonlinear and soft matter physics
N2  - A symmetry-breaking mechanism is investigated that creates bistability between fully and partially synchronized states in oscillator networks. Two populations of oscillators with unimodal frequency distribution and different amplitudes, in the presence of weak global coupling, are shown to simplify to a modular network with asymmetrical coupling. With increasing the coupling strength, a synchronization transition is observed with an isolated fully synchronized state. The results are interpreted theoretically in the thermodynamic limit and confirmed in experiments with chemical oscillators.
Y1  - 2021
U6  - https://doi.org/10.1103/PhysRevE.104.L022202
SN  - 2470-0045
SN  - 2470-0053
VL  - 104
IS  - 2
PB  - American Physical Society
CY  - Melville, NY
ER  - 
TY  - JOUR
A1  - Meyer, Dominique M.-A.
A1  - Pohl, Martin
A1  - Petrov, Miroslav
A1  - Egberts, Kathrin
T1  - Mixing of materials in magnetized core-collapse supernova remnants
JF  - Monthly notices of the Royal Astronomical Society
N2  - Core-collapse supernova remnants are structures of the interstellar medium (ISM) left behind the explosive death of most massive stars ( ?40 M-?). Since they result in the expansion of the supernova shock wave into the gaseous environment shaped by the star's wind history, their morphology constitutes an insight into the past evolution of their progenitor star. Particularly, fast-mo ving massiv e stars can produce asymmetric core-collapse superno va remnants. We inv estigate the mixing of materials in core-collapse supernova remnants generated by a moving massive 35 M-? star, in a magnetized ISM. Stellar rotation and the wind magnetic field are time-dependently included into the models which follow the entire evolution of the stellar surroundings from the zero-age main-sequence to 80 kyr after the supernova explosion. It is found that very little main-sequence material is present in remnants from moving stars, that the Wolf-Rayet wind mixes very efficiently within the 10 kyr after the explosion, while the red supergiant material is still unmixed by 30 per cent within 50 kyr after the supernova. Our results indicate that the faster the stellar motion, the more complex the internal organization of the supernova remnant and the more ef fecti ve the mixing of ejecta therein. In contrast, the mixing of stellar wind material is only weakly affected by progenitor motion, if at all.
KW  - ISM : supernova remnants
KW  - (magnetohydrodynamics) MHD
KW  - stars evolution
KW  - stars: massive
Y1  - 2023
U6  - https://doi.org/10.1093/mnras/stad906
SN  - 0035-8711
SN  - 1365-2966
VL  - 521
IS  - 4
SP  - 5354
EP  - 5371
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Davidsen, Joern
A1  - Kwiatek, Grzegorz
A1  - Charalampidou, Elli-Maria
A1  - Goebel, Thomas H. W.
A1  - Stanchits, Sergei
A1  - Rueck, Marc
A1  - Dresen, Georg
T1  - Triggering Processes in Rock Fracture
JF  - Physical review letters
N2  - We study triggering processes in triaxial compression experiments under a constant displacement rate on sandstone and granite samples using spatially located acoustic emission events and their focal mechanisms. We present strong evidence that event-event triggering plays an important role in the presence of large-scale or macrocopic imperfections, while such triggering is basically absent if no significant imperfections are present. In the former case, we recover all established empirical relations of aftershock seismicity including the Gutenberg-Richter relation, a modified version of the Omori-Utsu relation and the productivity relation-despite the fact that the activity is dominated by compaction-type events and triggering cascades have a swarmlike topology. For the Gutenberg-Richter relations, we find that the b value is smaller for triggered events compared to background events. Moreover, we show that triggered acoustic emission events have a focal mechanism much more similar to their associated trigger than expected by chance.
Y1  - 2017
U6  - https://doi.org/10.1103/PhysRevLett.119.068501
SN  - 0031-9007
SN  - 1079-7114
VL  - 119
PB  - American Physical Society
CY  - College Park
ER  - 
TY  - JOUR
A1  - Kretzschmar, Mirjam E.
A1  - Ashby, Ben
A1  - Fearon, Elizabeth
A1  - Overton, Christopher E.
A1  - Panovska-Griffiths, Jasmina
A1  - Pellis, Lorenzo
A1  - Quaife, Matthew
A1  - Rozhnova, Ganna
A1  - Scarabel, Francesca
A1  - Stage, Helena B.
A1  - Swallow, Ben
A1  - Thompson, Robin N.
A1  - Tildesley, Michael J.
A1  - Villela, Daniel Campos
T1  - Challenges for modelling interventions for future pandemics
JF  - Epidemics
N2  - Mathematical modelling and statistical inference provide a framework to evaluate different non-pharmaceutical and pharmaceutical interventions for the control of epidemics that has been widely used during the COVID-19 pandemic. In this paper, lessons learned from this and previous epidemics are used to highlight the challenges for future pandemic control. We consider the availability and use of data, as well as the need for correct parameterisation and calibration for different model frameworks. We discuss challenges that arise in describing and distinguishing between different interventions, within different modelling structures, and allowing both within and between host dynamics. We also highlight challenges in modelling the health economic and political aspects of interventions. Given the diversity of these challenges, a broad variety of interdisciplinary expertise is needed to address them, combining mathematical knowledge with biological and social insights, and including health economics and communication skills. Addressing these challenges for the future requires strong cross disciplinary collaboration together with close communication between scientists and policy makers.
KW  - Mathematical models
KW  - Pandemics
KW  - Pharmaceutical interventions
KW  - Non-pharmaceutical interventions
KW  - Policy support
Y1  - 2022
U6  - https://doi.org/10.1016/j.epidem.2022.100546
SN  - 1755-4365
SN  - 1878-0067
VL  - 38
PB  - Elsevier
CY  - Amsterdam
ER  - 
TY  - THES
A1  - Schlemm, Tanja
T1  - The marine ice cliff instability of the Antarctic ice sheet
T1  - Die marine Eisklippeninstabilität des antarktischen Eisschildes
BT  - a theory of mélange-buttressed cliff calving and its application in the Parallel Ice Sheet Model
BT  - eine Theorie des Mélange-gebremsten Klippenkalbens und ihre Anwendung im Parallel Ice Sheet Model
N2  - The Antarctic ice sheet is the largest freshwater reservoir worldwide. If it were to melt completely, global sea levels would rise by about 58 m. Calculation of projections of the Antarctic contribution to sea level rise under global warming conditions is an ongoing effort which
yields large ranges in predictions. Among the reasons for this are uncertainties related to the physics of ice sheet modeling. These
uncertainties include two processes that could lead to runaway ice retreat: the Marine Ice Sheet Instability (MISI), which causes rapid grounding line retreat on retrograde bedrock, and the Marine Ice Cliff Instability (MICI), in which tall ice cliffs become unstable and calve off, exposing even taller ice cliffs.
In my thesis, I investigated both marine instabilities (MISI and MICI) using the Parallel Ice Sheet Model (PISM), with a focus on MICI.
N2  - Der antarktische Eisschild ist das größte Süßwasserreservoir der Welt. Würde er vollständig schmelzen, würde der globale Meeresspiegel um etwa 58 m ansteigen. Die Ermittlung von Prognosen über den Beitrag der Antarktis zum Anstieg des Meeresspiegels infolge der globalen Erwärmung ist ein fortlaufender Prozess, der große Unterschiede in den Vorhersagen zur Folge hat. Einer der Gründe dafür sind Ungewissheiten im Zusammenhang mit der Physik der Eisschildmodellierung. Zu diesen Unsicherheiten gehören zwei Prozesse, die zu einem unkontrollierten Eisrückzug führen könnten:
die Marine Ice Sheet Instability (MISI), die zu einem schnellen Rückzug der Grundlinie auf rückläufigem Grundgestein führt, und die Marine Ice Cliff Instability (MICI), bei der hohe Eisklippen instabil werden und abkalben, wodurch noch höhere Eisklippen freigelegt werden.
In meiner Dissertation untersuchte ich beide marinen Instabilitäten (MISI und MICI) mit Hilfe des Parallel Ice Sheet Model (PISM), wobei der Schwerpunkt auf MICI lag.
KW  - Antarctica
KW  - ice sheet modelling
KW  - iceberg calving
KW  - Antarktis
KW  - Eisschildmodellierung
KW  - Eisbergkalbung
Y1  - 2022
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-586333
ER  - 
TY  - THES
A1  - Kuhla, Kilian
T1  - Impact, distribution, and adaptation
T1  - Auswirkung, Verteilung und Anpassung
BT  - how weather extremes threaten the economic network
BT  - wie Wetterextreme das ökonomische Netzwerk bedrohen
N2  - Weather extremes pose a persistent threat to society on multiple layers. Besides an average of ~37,000 deaths per year, climate-related disasters cause destroyed properties and impaired economic activities, eroding people's livelihoods and prosperity. While global temperature rises – caused by anthropogenic greenhouse gas emissions – the direct impacts of climatic extreme events increase and will further intensify without proper adaptation measures. Additionally, weather extremes do not only have local direct effects. Resulting economic repercussions can propagate either upstream or downstream along trade chains causing indirect effects. One approach to analyze these indirect effects within the complex global supply network is the agent-based model Acclimate. Using and extending this loss-propagation model, I focus in this thesis on three aspects of the relation between weather extremes and economic repercussions.

First, extreme weather events cause direct impacts on local economic performance. I compute daily local direct output loss time series of heat stress, river floods, tropical cyclones, and their consecutive occurrence using (near-future) climate projection ensembles. These regional impacts are estimated based on physical drivers and local productivity distribution. Direct effects of the aforementioned disaster categories are widely heterogeneous concerning regional and temporal distribution. As well, their intensity changes differently under future warming. Focusing on the hurricane-impacted capital, I find that long-term growth losses increase with higher heterogeneity of a shock ensemble. 

Second, repercussions are sectorally and regionally distributed via economic ripples within the trading network, causing higher-order effects. I use Acclimate to identify three phases of those economic ripples. Furthermore, I compute indirect impacts and analyze overall regional and global production and consumption changes. Regarding heat stress, global consumer losses double while direct output losses increase by a factor 1.5 between 2000 – 2039. In my research I identify the effect of economic ripple resonance and introduce it to climate impact research. This effect occurs if economic ripples of consecutive disasters overlap, which increases economic responses such as an enhancement of consumption losses. These loss enhancements can even be more amplified with increasing direct output losses, e.g. caused by climate crises.  

Transport disruptions can cause economic repercussions as well. For this, I extend the model Acclimate with a geographical transportation route and expand the decision horizon of economic agents. Using this, I show that policy-induced sudden trade restrictions (e.g. a no-deal Brexit) can significantly reduce the longer-term economic prosperity of affected regions. Analyses of transportation disruptions in typhoon seasons indicate that severely affected regions must reduce production as demand falls during a storm. Substituting suppliers may compensate for fluctuations at the beginning of the storm, which fails for prolonged disruptions.

Third, possible coping mechanisms and adaptation strategies arise from direct and indirect economic responses to weather extremes. Analyzing annual trade changes due to typhoon-induced transport disruptions depict that overall exports rise. This trade resilience increases with higher network node diversification. Further, my research shows that a basic insurance scheme may diminish hurricane-induced long-term growth losses due to faster reconstruction in disasters aftermaths. I find that insurance coverage could be an economically reasonable coping scheme towards higher losses caused by the climate crisis. Indirect effects within the global economic network from weather extremes indicate further adaptation possibilities. For one, diversifying linkages reduce the hazard of sharp price increases. Next to this, close economic interconnections with regions that do not share the same extreme weather season can be economically beneficial in the medium run. Furthermore, economic ripple resonance effects should be considered while computing costs. Overall, an increase in local adaptation measures reduces economic ripples within the trade network and possible losses elsewhere. In conclusion, adaptation measures are necessary and potential present, but it seems rather not possible to avoid all direct or indirect losses.

As I show in this thesis, dynamical modeling gives valuable insights into how direct and indirect economic impacts arise from different categories of weather extremes. Further, it highlights the importance of resolving individual extremes and reflecting amplifying effects caused by incomplete recovery or consecutive disasters.
N2  - Wetterextreme stellen für die Gesellschaft eine anhaltende Bedrohung auf mehreren Ebenen dar. Neben durchschnittlich ~37.000 Todesfällen pro Jahr verursachen meteorologische Katastrophen Eigentumsschäden und Wirtschaftsbeeinträchtigungen, wodurch die Lebensgrundlagen und der Wohlstand der Menschen untergraben werden. Während die globale Temperatur – verursacht durch anthropogene Treibhausgasemissionen – ansteigt, nehmen die direkten Auswirkungen klimatischer Extremereignisse zu und werden sich ohne geeignete Anpassungsmaßnahmen weiter verstärken. 
Hinzu kommt, dass Wetterextreme nicht nur lokal direkte Schäden anrichten, sondern sich wetterbedingte wirtschaftliche Auswirkungen auch entlang der Handelsketten ausbreiten und so indirekte Effekte nach sich ziehen. Ein Ansatz zur Analyse dieser indirekten Auswirkungen innerhalb des komplexen globalen Versorgungsnetzes ist das agentenbasierte Modell Acclimate. 
In meiner Dissertation verwende und erweitere ich dieses Schadenspropagationsmodell, um drei Aspekte der Beziehung zwischen Wetterextremen und wirtschaftlichen Auswirkungen zu untersuchen.

Erstens verursachen extreme Wetterereignisse direkte Schäden in lokaler Wirtschaftsleistung. Die regionalen Auswirkungen werden auf der Grundlage von physikalischen Faktoren und lokalen Produktivitätsverteilungen kalkuliert. Ich berechne tägliche Zeitreihen lokaler Produktionsverluste durch Hitzestress, Überschwemmungen, tropische Wirbelstürme und deren konsekutives Auftreten unter Verwendung von Klimaprojektionsensembles. Die direkten Auswirkungen der oben genannten Katastrophenkategorien sind sehr heterogen in Bezug auf die regionale und zeitliche Verteilung. Ebenso ändert sich ihre Stärke unterschiedlich unter zukünftiger Erwärmung. Meine Forschungsergebnisse zeigen, dass Kapitalstock, welcher von Wirbelstürmen beschädigt ist, langfristige Wachstumsverluste verursacht. Dabei nehmen die Verluste zu, wenn die Heterogenität der Schocks steigt.

Zweitens werden die wetterbedingten Auswirkungen durch wirtschaftliche Wellen innerhalb des Handelsnetzes auf verschiedene Wirtschaftssektoren und Regionen verteilt. In meiner Dissertation, untersuche ich die wirtschaftlichen Wellen mittels Acclimate und mache dabei drei Wellenphasen aus. Darüber hinaus berechne ich indirekte Auswirkungen und analysiere die regionalen und globalen Produktionsveränderungen sowie die Auswirkungen auf Konsumierende. Für letztere verdoppeln sich zwischen 2000 und 2039 die weltweiten Verluste durch Hitzestress, während im selben Zeitraum die direkten Produktionsverluste nur um den Faktor 1.5 steigen. Im Zuge meiner Forschung identifiziere ich den Effekt der ökonomischen Wellenresonanz und führe ihn in die Klimafolgenforschung ein. Dieser Effekt tritt auf, wenn sich die ökonomischen Wellen aufeinanderfolgender Katastrophen überlagern, was wirtschaftliche Reaktionen intensiviert wie beispielsweise eine Steigerung der Konsumverluste. Diese Dynamik der Verluste kann durch zunehmende direkte Produktionsverluste, hervorgerufen etwa durch den Klimawandel, noch verstärkt werden. 

Auch Handelsunterbrechungen können wirtschaftliche Auswirkungen haben. Um diese zu berechnen, erweitere ich das Modell Acclimate um ein geografisches Transportnetzwerk und weite den Entscheidungshorizont der Wirtschaftsakteure aus. Politisch bedingte plötzliche Handelsbeschränkungen (z. B. ein No-Deal-Brexit) können den längerfristigen wirtschaftlichen Wohlstand der betroffenen Regionen erheblich verringern. Analysen von Transportunterbrechungen in der Taifunsaison zeigen, dass stark betroffene Regionen ihre Produktionen reduzieren müssen, wenn die Nachfrage während eines Sturms sinkt. Zu Beginn eines Sturms können Handelsschwankungen durch alternative Lieferanten ausgeglichen werden, was jedoch bei längeren Unterbrechungen nicht mehr gelingt.

Drittens ergeben sich mögliche Anpassungsmechanismen und -strategien aus direkten und indirekten wirtschaftlichen Reaktionen auf Wetterextreme. Die Analyse der jährlichen Handelsveränderungen in der Taifunsaison zeigt, dass Exporte insgesamt zunehmen. Diese Widerstandsfähigkeit des Handels wächst mit einer höheren Diversifizierung der Handelspartner. Weiterhin zeigt meine Forschung an Wirtschaftswachstumsmodellen, dass ein Versicherungssystem langfristige Wachstumsverluste, verursacht durch Tropenstürme, durch schnelleren Wiederaufbau verringern kann. Ich komme zu dem Schluss, dass ein Versicherungsschutz eine wirtschaftlich sinnvolle Anpassungsstrategie gegenüber höheren Schäden durch die Klimakrise sein kann. Ebenso weisen indirekte Auswirkungen von Wetterextremen innerhalb des globalen Wirtschaftsnetzes auf weitere Anpassungsmöglichkeiten hin. Zunächst vermindert eine diversifizierte Vernetzung die Gefahr eines starken Preisanstiegs. Ebenso kann eine enge wirtschaftliche Verflechtung von Regionen, die nicht dieselbe Unwettersaison haben, mittelfristig wirtschaftlich vorteilhaft sein. Weiterhin sollten bei der Berechnung der Kosten wirtschaftliche Resonanzeffekte berücksichtigt werden. Eine Verstärkung der lokalen Anpassungsmaßnahmen verringert die Amplitude ökonomischer Wellen und damit auch potentielle Verluste in anderen Regionen. Insgesamt sind Anpassungsmaßnahmen notwendig, aber es scheint trotz dieser nicht möglich zu sein, alle direkten oder indirekten Verluste zu vermeiden.

Wie ich in meiner Arbeit darlege, gibt die dynamische Modellierung wertvolle Einblicke in die Art und Weise, wie direkte und indirekte wirtschaftliche Auswirkungen durch verschiedene Wetterextreme entstehen. Darüber hinaus wird deutlich, wie wichtig es ist, einzelne Extremereignisse aufzulösen und Verstärkungseffekte zu berücksichtigen, die durch unvollständigen Wiederaufbau oder aufeinanderfolgende Katastrophen verursacht werden.
KW  - climate change
KW  - weather extremes
KW  - macro-economic modelling
KW  - network theory
KW  - economic network
KW  - Klimawandel
KW  - Wetterextreme
KW  - Makroökonomische Modellierung
KW  - Netzwerktheorie
KW  - Ökonomisches Netzwerk
Y1  - 2022
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-552668
ER  - 
TY  - JOUR
A1  - Seroussi, Helene
A1  - Nowicki, Sophie
A1  - Simon, Erika
A1  - Abe-Ouchi, Ayako
A1  - Albrecht, Torsten
A1  - Brondex, Julien
A1  - Cornford, Stephen
A1  - Dumas, Christophe
A1  - Gillet-Chaulet, Fabien
A1  - Goelzer, Heiko
A1  - Golledge, Nicholas R.
A1  - Gregory, Jonathan M.
A1  - Greve, Ralf
A1  - Hoffman, Matthew J.
A1  - Humbert, Angelika
A1  - Huybrechts, Philippe
A1  - Kleiner, Thomas
A1  - Larourl, Eric
A1  - Leguy, Gunter
A1  - Lipscomb, William H.
A1  - Lowry, Daniel
A1  - Mengel, Matthias
A1  - Morlighem, Mathieu
A1  - Pattyn, Frank
A1  - Payne, Anthony J.
A1  - Pollard, David
A1  - Price, Stephen F.
A1  - Quiquet, Aurelien
A1  - Reerink, Thomas J.
A1  - Reese, Ronja
A1  - Rodehacke, Christian B.
A1  - Schlegel, Nicole-Jeanne
A1  - Shepherd, Andrew
A1  - Sun, Sainan
A1  - Sutter, Johannes
A1  - Van Breedam, Jonas
A1  - van de Wal, Roderik S. W.
A1  - Winkelmann, Ricarda
A1  - Zhang, Tong
T1  - initMIP-Antarctica
BT  - an ice sheet model initialization experiment of ISMIP6
JF  - The Cryosphere : TC ; an interactive open access journal of the European Geosciences Union
N2  - Ice sheet numerical modeling is an important tool to estimate the dynamic contribution of the Antarctic ice sheet to sea level rise over the coming centuries. The influence of initial conditions on ice sheet model simulations, however, is still unclear. To better understand this influence, an initial state intercomparison exercise (initMIP) has been developed to compare, evaluate, and improve initialization procedures and estimate their impact on century-scale simulations. initMlP is the first set of experiments of the Ice Sheet Model Intercomparison Project for CMIP6 (ISMIP6), which is the primary Coupled Model Intercomparison Project Phase 6 (CMIP6) activity focusing on the Greenland and Antarctic ice sheets. Following initMlP-Greenland, initMlP-Antarctica has been designed to explore uncertainties associated with model initialization and spin-up and to evaluate the impact of changes in external forcings. Starting from the state of the Antarctic ice sheet at the end of the initialization procedure, three forward experiments are each run for 100 years: a control run, a run with a surface mass balance anomaly, and a run with a basal melting anomaly beneath floating ice. This study presents the results of initMlP-Antarctica from 25 simulations performed by 16 international modeling groups. The submitted results use different initial conditions and initialization methods, as well as ice flow model parameters and reference external forcings. We find a good agreement among model responses to the surface mass balance anomaly but large variations in responses to the basal melting anomaly. These variations can be attributed to differences in the extent of ice shelves and their upstream tributaries, the numerical treatment of grounding line, and the initial ocean conditions applied, suggesting that ongoing efforts to better represent ice shelves in continental-scale models should continue.
Y1  - 2019
U6  - https://doi.org/10.5194/tc-13-1441-2019
SN  - 1994-0416
SN  - 1994-0424
VL  - 13
IS  - 5
SP  - 1441
EP  - 1471
PB  - Copernicus
CY  - Göttingen
ER  - 
TY  - JOUR
A1  - Reese, Ronja
A1  - Albrecht, Torsten
A1  - Mengel, Matthias
A1  - Asay-Davis, Xylar
A1  - Winkelmann, Ricarda
T1  - Antarctic sub-shelf melt rates via PICO
JF  - The Cryosphere : TC ; an interactive open access journal of the European Geosciences Union
N2  - Ocean-induced melting below ice shelves is one of the dominant drivers for mass loss from the Antarctic Ice Sheet at present. An appropriate representation of sub-shelf melt rates is therefore essential for model simulations of marine-based ice sheet evolution. Continental-scale ice sheet models often rely on simple melt-parameterizations, in particular for long-term simulations, when fully coupled ice-ocean interaction becomes computationally too expensive. Such parameterizations can account for the influence of the local depth of the ice-shelf draft or its slope on melting. However, they do not capture the effect of ocean circulation underneath the ice shelf. Here we present the Potsdam Ice-shelf Cavity mOdel (PICO), which simulates the vertical overturning circulation in ice-shelf cavities and thus enables the computation of sub-shelf melt rates consistent with this circulation. PICO is based on an ocean box model that coarsely resolves ice shelf cavities and uses a boundary layer melt formulation. We implement it as a module of the Parallel Ice Sheet Model (PISM) and evaluate its performance under present-day conditions of the Southern Ocean. We identify a set of parameters that yield two-dimensional melt rate fields that qualitatively reproduce the typical pattern of comparably high melting near the grounding line and lower melting or refreezing towards the calving front. PICO captures the wide range of melt rates observed for Antarctic ice shelves, with an average of about 0.1 ma(-1) for cold sub-shelf cavities, for example, underneath Ross or Ronne ice shelves, to 16 ma(-1) for warm cavities such as in the Amundsen Sea region. This makes PICO a computationally feasible and more physical alternative to melt parameterizations purely based on ice draft geometry.
Y1  - 2018
U6  - https://doi.org/10.5194/tc-12-1969-2018
SN  - 1994-0416
SN  - 1994-0424
VL  - 12
IS  - 6
SP  - 1969
EP  - 1985
PB  - Copernicus
CY  - Göttingen
ER  - 
TY  - JOUR
A1  - Levermann, Anders
A1  - Winkelmann, Ricarda
A1  - Nowicki, S.
A1  - Fastook, J. L.
A1  - Frieler, Katja
A1  - Greve, R.
A1  - Hellmer, H. H.
A1  - Martin, M. A.
A1  - Meinshausen, Malte
A1  - Mengel, Matthias
A1  - Payne, A. J.
A1  - Pollard, D.
A1  - Sato, T.
A1  - Timmermann, R.
A1  - Wang, Wei Li
A1  - Bindschadler, Robert A.
T1  - Projecting antarctic ice discharge using response functions from SeaRISE ice-sheet models
JF  - Earth system dynamics
N2  - The largest uncertainty in projections of future sea-level change results from the potentially changing dynamical ice discharge from Antarctica. Basal ice-shelf melting induced by a warming ocean has been identified as a major cause for additional ice flow across the grounding line. Here we attempt to estimate the uncertainty range of future ice discharge from Antarctica by combining uncertainty in the climatic forcing, the oceanic response and the ice-sheet model response. The uncertainty in the global mean temperature increase is obtained from historically constrained emulations with the MAGICC-6.0 (Model for the Assessment of Greenhouse gas Induced Climate Change) model. The oceanic forcing is derived from scaling of the subsurface with the atmospheric warming from 19 comprehensive climate models of the Coupled Model Intercomparison Project (CMIP-5) and two ocean models from the EU-project Ice2Sea. The dynamic ice-sheet response is derived from linear response functions for basal ice-shelf melting for four different Antarctic drainage regions using experiments from the Sea-level Response to Ice Sheet Evolution (SeaRISE) intercomparison project with five different Antarctic ice-sheet models. The resulting uncertainty range for the historic Antarctic contribution to global sea-level rise from 1992 to 2011 agrees with the observed contribution for this period if we use the three ice-sheet models with an explicit representation of ice-shelf dynamics and account for the time-delayed warming of the oceanic subsurface compared to the surface air temperature. The median of the additional ice loss for the 21st century is computed to 0.07 m (66% range: 0.02-0.14 m; 90% range: 0.0-0.23 m) of global sea-level equivalent for the low-emission RCP-2.6 (Representative Concentration Pathway) scenario and 0.09 m (66% range: 0.04-0.21 m; 90% range: 0.01-0.37 m) for the strongest RCP-8.5. Assuming no time delay between the atmospheric warming and the oceanic subsurface, these values increase to 0.09 m (66% range: 0.04-0.17 m; 90% range: 0.02-0.25 m) for RCP-2.6 and 0.15 m (66% range: 0.07-0.28 m; 90% range: 0.04-0.43 m) for RCP-8.5. All probability distributions are highly skewed towards high values. The applied ice-sheet models are coarse resolution with limitations in the representation of grounding-line motion. Within the constraints of the applied methods, the uncertainty induced from different ice-sheet models is smaller than that induced by the external forcing to the ice sheets.
Y1  - 2014
U6  - https://doi.org/10.5194/esd-5-271-2014
SN  - 2190-4979
SN  - 2190-4987
VL  - 5
IS  - 2
SP  - 271
EP  - 293
PB  - Copernicus
CY  - Göttingen
ER  - 
TY  - JOUR
A1  - Steffen, Will
A1  - Röckstrom, Johan
A1  - Richardson, Katherine
A1  - Lenton, Timothy M.
A1  - Folke, Carl
A1  - Liverman, Diana
A1  - Summerhayes, Colin P.
A1  - Barnosky, Anthony D.
A1  - Cornell, Sarah E.
A1  - Crucifix, Michel
A1  - Donges, Jonathan
A1  - Fetzer, Ingo
A1  - Lade, Steven J.
A1  - Scheffer, Marten
A1  - Winkelmann, Ricarda
A1  - Schellnhuber, Hans Joachim
T1  - Trajectories of the Earth System in the Anthropocene
JF  - Proceedings of the National Academy of Sciences of the United States of America
N2  - We explore the risk that self-reinforcing feedbacks could push the Earth System toward a planetary threshold that, if crossed, could prevent stabilization of the climate at intermediate temperature rises and cause continued warming on a "Hothouse Earth" pathway even as human emissions are reduced. Crossing the threshold would lead to a much higher global average temperature than any interglacial in the past 1.2 million years and to sea levels significantly higher than at any time in the Holocene. We examine the evidence that such a threshold might exist and where it might be. If the threshold is crossed, the resulting trajectory would likely cause serious disruptions to ecosystems, society, and economies. Collective human action is required to steer the Earth System away from a potential threshold and stabilize it in a habitable interglacial-like state. Such action entails stewardship of the entire Earth System-biosphere, climate, and societies-and could include decarbonization of the global economy, enhancement of biosphere carbon sinks, behavioral changes, technological innovations, new governance arrangements, and transformed social values.
KW  - Earth System trajectories
KW  - climate change
KW  - Anthropocene
KW  - biosphere feedbacks
KW  - tipping elements
Y1  - 2018
U6  - https://doi.org/10.1073/pnas.1810141115
SN  - 0027-8424
VL  - 115
IS  - 33
SP  - 8252
EP  - 8259
PB  - National Acad. of Sciences
CY  - Washington
ER  - 
TY  - JOUR
A1  - Clark, Peter U.
A1  - Shakun, Jeremy D.
A1  - Marcott, Shaun A.
A1  - Mix, Alan C.
A1  - Eby, Michael
A1  - Kulp, Scott
A1  - Levermann, Anders
A1  - Milne, Glenn A.
A1  - Pfister, Patrik L.
A1  - Santer, Benjamin D.
A1  - Schrag, Daniel P.
A1  - Solomon, Susan
A1  - Stocker, Thomas F.
A1  - Strauss, Benjamin H.
A1  - Weaver, Andrew J.
A1  - Winkelmann, Ricarda
A1  - Archer, David
A1  - Bard, Edouard
A1  - Goldner, Aaron
A1  - Lambeck, Kurt
A1  - Pierrehumbert, Raymond T.
A1  - Plattner, Gian-Kasper
T1  - Consequences of twenty-first-century policy for multi-millennial climate
and sea-level change
JF  - Nature climate change
N2  - Most of the policy debate surrounding the actions needed to mitigate and adapt to anthropogenic climate change has been framed by observations of the past 150 years as well as climate and sea-level projections for the twenty-first century. The focus on this 250-year window, however, obscures some of the most profound problems associated with climate change. Here, we argue that the twentieth and twenty-first centuries, a period during which the overwhelming majority of human-caused carbon emissions are likely to occur, need to be placed into a long-term context that includes the past 20 millennia, when the last Ice Age ended and human civilization developed, and the next ten millennia, over which time the projected impacts of anthropogenic climate change will grow and persist. This long-term perspective illustrates that policy decisions made in the next few years to decades will have profound impacts on global climate, ecosystems and human societies - not just for this century, but for the next ten millennia and beyond.
Y1  - 2016
U6  - https://doi.org/10.1038/NCLIMATE2923
SN  - 1758-678X
SN  - 1758-6798
VL  - 6
SP  - 360
EP  - 369
PB  - Nature Publ. Group
CY  - London
ER  - 
TY  - JOUR
A1  - Ciemer, Catrin
A1  - Boers, Niklas
A1  - Hirota, Marina
A1  - Kurths, Jürgen
A1  - Müller-Hansen, Finn
A1  - Oliveira, Rafael S.
A1  - Winkelmann, Ricarda
T1  - Higher resilience to climatic disturbances in tropical vegetation exposed to more variable rainfall
JF  - Nature geoscience
N2  - With ongoing global warming, the amount and frequency of precipitation in the tropics is projected to change substantially. While it has been shown that tropical forests and savannahs are sustained within the same intermediate mean annual precipitation range, the mechanisms that lead to the resilience of these ecosystems are still not fully understood. In particular, the long-term impact of rainfall variability on resilience is as yet unclear. Here we present observational evidence that both tropical forest and savannah exposed to a higher rainfall variability-in particular on interannual scales-during their long-term past are overall more resilient against climatic disturbances. Based on precipitation and tree cover data in the Brazilian Amazon basin, we constructed potential landscapes that enable us to systematically measure the resilience of the different ecosystems. Additionally, we infer that shifts from forest to savannah due to decreasing precipitation in the future are more likely to occur in regions with a precursory lower rainfall variability. Long-term rainfall variability thus needs to be taken into account in resilience analyses and projections of vegetation response to climate change.
Y1  - 2019
U6  - https://doi.org/10.1038/s41561-019-0312-z
SN  - 1752-0894
SN  - 1752-0908
VL  - 12
IS  - 3
SP  - 174
EP  - 179
PB  - Nature Publ. Group
CY  - New York
ER  - 
TY  - JOUR
A1  - Ganopolski, A.
A1  - Winkelmann, Ricarda
A1  - Schellnhuber, Hans Joachim
T1  - Critical insolation-CO2 relation for diagnosing past and future glacial inception
JF  - Nature : the international weekly journal of science
N2  - The past rapid growth of Northern Hemisphere continental ice sheets, which terminated warm and stable climate periods, is generally attributed to reduced summer insolation in boreal latitudes(1-3). Yet such summer insolation is near to its minimum at present(4), and there are no signs of a new ice age(5). This challenges our understanding of the mechanisms driving glacial cycles and our ability to predict the next glacial inception(6). Here we propose a critical functional relationship between boreal summer insolation and global carbon dioxide (CO2) concentration, which explains the beginning of the past eight glacial cycles and might anticipate future periods of glacial inception. Using an ensemble of simulations generated by an Earth system model of intermediate complexity constrained by palaeoclimatic data, we suggest that glacial inception was narrowly missed before the beginning of the Industrial Revolution. The missed inception can be accounted for by the combined effect of relatively high late-Holocene CO2 concentrations and the low orbital eccentricity of the Earth(7). Additionally, our analysis suggests that even in the absence of human perturbations no substantial build-up of ice sheets would occur within the next several thousand years and that the current interglacial would probably last for another 50,000 years. However, moderate anthropogenic cumulative CO2 emissions of 1,000 to 1,500 gigatonnes of carbon will postpone the next glacial inception by at least 100,000 years(8,9). Our simulations demonstrate that under natural conditions alone the Earth system would be expected to remain in the present delicately balanced interglacial climate state, steering clear of both large-scale glaciation of the Northern Hemisphere and its complete deglaciation, for an unusually long time.
Y1  - 2016
U6  - https://doi.org/10.1038/nature16494
SN  - 0028-0836
SN  - 1476-4687
VL  - 529
SP  - 200
EP  - U159
PB  - Nature Publ. Group
CY  - London
ER  - 
TY  - JOUR
A1  - Reese, Ronja
A1  - Winkelmann, Ricarda
A1  - Gudmundsson, Gudmundur Hilmar
T1  - Grounding-line flux formula applied as a flux condition in numerical simulations fails for buttressed Antarctic ice streams
JF  - The Cryosphere : TC ; an interactive open access journal of the European Geosciences Union
N2  - Currently, several large-scale ice-flow models impose a condition on ice flux across grounding lines using an analytically motivated parameterisation of grounding-line flux. It has been suggested that employing this analytical expression alleviates the need for highly resolved computational domains around grounding lines of marine ice sheets. While the analytical flux formula is expected to be accurate in an unbuttressed flow-line setting, its validity has hitherto not been assessed for complex and realistic geometries such as those of the Antarctic Ice Sheet. Here the accuracy of this analytical flux formula is tested against an optimised ice flow model that uses a highly resolved computational mesh around the Antarctic grounding lines. We find that when applied to the Antarctic Ice Sheet the analytical expression provides inaccurate estimates of ice fluxes for almost all grounding lines. Furthermore, in many instances direct application of the analytical formula gives rise to unphysical complex-valued ice fluxes. We conclude that grounding lines of the Antarctic Ice Sheet are, in general, too highly buttressed for the analytical parameterisation to be of practical value for the calculation of grounding-line fluxes.
Y1  - 2018
U6  - https://doi.org/10.5194/tc-12-3229-2018
SN  - 1994-0416
SN  - 1994-0424
VL  - 12
IS  - 10
SP  - 3229
EP  - 3242
PB  - Copernicus
CY  - Göttingen
ER  - 
TY  - JOUR
A1  - Ciemer, Catrin
A1  - Rehm, Lars
A1  - Kurths, Jürgen
A1  - Donner, Reik Volker
A1  - Winkelmann, Ricarda
A1  - Boers, Niklas
T1  - An early-warning indicator for Amazon droughts exclusively based on tropical Atlantic sea surface temperatures
JF  - Environmental Research Letters
N2  - Droughts in tropical South America have an imminent and severe impact on the Amazon rainforest and affect the livelihoods of millions of people. Extremely dry conditions in Amazonia have been previously linked to sea surface temperature (SST) anomalies in the adjacent tropical oceans. Although the sources and impacts of such droughts have been widely studied, establishing reliable multi-year lead statistical forecasts of their occurrence is still an ongoing challenge. Here, we further investigate the relationship between SST and rainfall anomalies using a complex network approach. We identify four ocean regions which exhibit the strongest overall SST correlations with central Amazon rainfall, including two particularly prominent regions in the northern and southern tropical Atlantic. Based on the time-dependent correlation between SST anomalies in these two regions alone, we establish a new early-warning method for droughts in the central Amazon basin and demonstrate its robustness in hindcasting past major drought events with lead-times up to 18 months.
KW  - complex networks
KW  - droughts
KW  - prediction
KW  - Amazon rainforest
Y1  - 2019
VL  - 15
IS  - 9
PB  - IOP - Institute of Physics Publishing
CY  - Bristol
ER  - 
TY  - JOUR
A1  - Frieler, Katja
A1  - Clark, Peter U.
A1  - He, Feng
A1  - Buizert, Christo
A1  - Reese, Ronja
A1  - Ligtenberg, Stefan R. M.
A1  - van den Broeke, Michiel R.
A1  - Winkelmann, Ricarda
A1  - Levermann, Anders
T1  - Consistent evidence of increasing Antarctic accumulation with warming
JF  - Nature climate change
N2  - Projections of changes in Antarctic Ice Sheet (AIS) surface mass balance indicate a negative contribution to sea level because of the expected increase in precipitation due to the higher moisture holding capacity of warmer air(1). Observations over the past decades, however, are unable to constrain the relation between temperature and accumulation changes because both are dominated by strong natural variability(2-5). Here we derive a consistent continental-scale increase in accumulation of approximately 5 +/- 1% K-1, through the assessment of ice-core data (spanning the large temperature change during the last deglaciation, 21,000 to 10,000 years ago), in combination with palaeo-simulations, future projections by 35 general circulation models (GCMs), and one high-resolution future simulation. The ice-core data and modelling results for the last deglaciation agree, showing uniform local sensitivities of similar to 6% K-1. The palaeo-simulation allows for a continental-scale aggregation of accumulation changes reaching 4.3% K-1. Despite the different timescales, these sensitivities agree with the multi-model mean of 6.1 +/- 2.6% K-1 (GCMprojections) and the continental-scale sensitivity of 4.9% K-1 (high-resolution future simulation). Because some of the mass gain of the AIS is offset by dynamical losses induced by accumulation(6,7), we provide a response function allowing projections of sea-level fall in terms of continental-scale accumulation changes that compete with surface melting and dynamical losses induced by other mechanisms(6,8,9).
Y1  - 2015
U6  - https://doi.org/10.1038/nclimate2574
SN  - 1758-678X
SN  - 1758-6798
VL  - 5
IS  - 4
SP  - 348
EP  - 352
PB  - Nature Publ. Group
CY  - London
ER  - 
TY  - JOUR
A1  - Levermann, Anders
A1  - Winkelmann, Ricarda
T1  - A simple equation for the melt elevation feedback of ice sheets
JF  - The Cryosphere : TC ; an interactive open access journal of the European Geosciences Union
N2  - In recent decades, the Greenland Ice Sheet has been losing mass and has thereby contributed to global sea-level rise. The rate of ice loss is highly relevant for coastal protection worldwide. The ice loss is likely to increase under future warming. Beyond a critical temperature threshold, a meltdown of the Greenland Ice Sheet is induced by the self-enforcing feedback between its lowering surface elevation and its increasing surface mass loss: the more ice that is lost, the lower the ice surface and the warmer the surface air temperature, which fosters further melting and ice loss. The computation of this rate so far relies on complex numerical models which are the appropriate tools for capturing the complexity of the problem. By contrast we aim here at gaining a conceptual understanding by deriving a purposefully simple equation for the self-enforcing feedback which is then used to estimate the melt time for different levels of warming using three observable characteristics of the ice sheet itself and its surroundings. The analysis is purely conceptual in nature. It is missing important processes like ice dynamics for it to be useful for applications to sea-level rise on centennial timescales, but if the volume loss is dominated by the feedback, the resulting logarithmic equation unifies existing numerical simulations and shows that the melt time depends strongly on the level of warming with a critical slow-down near the threshold: the median time to lose 10% of the present-day ice volume varies between about 3500 years for a temperature level of 0.5 degrees C above the threshold and 500 years for 5 degrees C. Unless future observations show a significantly higher melting sensitivity than currently observed, a complete meltdown is unlikely within the next 2000 years without significant ice-dynamical contributions.
Y1  - 2016
U6  - https://doi.org/10.5194/tc-10-1799-2016
SN  - 1994-0416
SN  - 1994-0424
VL  - 10
SP  - 1799
EP  - 1807
PB  - Copernicus
CY  - Göttingen
ER  - 
TY  - JOUR
A1  - Winkelmann, Ricarda
A1  - Martin, Maria A.
A1  - Haseloff, Monika
A1  - Albrecht, Torsten
A1  - Bueler, Ed
A1  - Khroulev, C.
A1  - Levermann, Anders
T1  - The Potsdam parallel ice sheet model (PISM-PIK) - Part 1: Model description
JF  - The Cryosphere : TC ; an interactive open access journal of the European Geosciences Union
N2  - We present the Potsdam Parallel Ice Sheet Model (PISM-PIK), developed at the Potsdam Institute for Climate Impact Research to be used for simulations of large-scale ice sheet-shelf systems. It is derived from the Parallel Ice Sheet Model (Bueler and Brown, 2009). Velocities are calculated by superposition of two shallow stress balance approximations within the entire ice covered region: the shallow ice approximation (SIA) is dominant in grounded regions and accounts for shear deformation parallel to the geoid. The plug-flow type shallow shelf approximation (SSA) dominates the velocity field in ice shelf regions and serves as a basal sliding velocity in grounded regions. Ice streams can be identified diagnostically as regions with a significant contribution of membrane stresses to the local momentum balance. All lateral boundaries in PISM-PIK are free to evolve, including the grounding line and ice fronts. Ice shelf margins in particular are modeled using Neumann boundary conditions for the SSA equations, reflecting a hydrostatic stress imbalance along the vertical calving face. The ice front position is modeled using a subgrid-scale representation of calving front motion (Albrecht et al., 2011) and a physically-motivated calving law based on horizontal spreading rates. The model is tested in experiments from the Marine Ice Sheet Model Intercomparison Project (MISMIP). A dynamic equilibrium simulation of Antarctica under present-day conditions is presented in Martin et al. (2011).
Y1  - 2011
U6  - https://doi.org/10.5194/tc-5-715-2011
SN  - 1994-0416
VL  - 5
IS  - 3
SP  - 715
EP  - 726
PB  - Copernicus
CY  - Göttingen
ER  - 
TY  - JOUR
A1  - Martin, Maria A.
A1  - Winkelmann, Ricarda
A1  - Haseloff, M.
A1  - Albrecht, Tanja
A1  - Bueler, Ed
A1  - Khroulev, C.
A1  - Levermann, Anders
T1  - The Potsdam parallel ice sheet model (PISM-PIK) - Part 2: Dynamic equilibrium simulation of the Antarctic ice sheet
JF  - The Cryosphere : TC ; an interactive open access journal of the European Geosciences Union
N2  - We present a dynamic equilibrium simulation of the ice sheet-shelf system on Antarctica with the Potsdam Parallel Ice Sheet Model (PISM-PIK). The simulation is initialized with present-day conditions for bed topography and ice thickness and then run to steady state with constant present-day surface mass balance. Surface temperature and sub-shelf basal melt distribution are parameterized. Grounding lines and calving fronts are free to evolve, and their modeled equilibrium state is compared to observational data. A physically-motivated calving law based on horizontal spreading rates allows for realistic calving fronts for various types of shelves. Steady-state dynamics including surface velocity and ice flux are analyzed for whole Antarctica and the Ronne-Filchner and Ross ice shelf areas in particular. The results show that the different flow regimes in sheet and shelves, and the transition zone between them, are captured reasonably well, supporting the approach of superposition of SIA and SSA for the representation of fast motion of grounded ice. This approach also leads to a natural emergence of sliding-dominated flow in stream-like features in this new 3-D marine ice sheet model.
Y1  - 2011
U6  - https://doi.org/10.5194/tc-5-727-2011
SN  - 1994-0416
VL  - 5
IS  - 3
SP  - 727
EP  - 740
PB  - Copernicus
CY  - Göttingen
ER  - 
TY  - THES
A1  - Reese, Ronja
T1  - The far reach of ice-shelf thinning in Antarctica
Y1  - 2018
ER  - 
TY  - THES
A1  - Winkelmann, Ricarda
T1  - The future sea-level contribution from antartica: projections of solid ice discharge
Y1  - 2012
CY  - Potsdam
ER  - 
TY  - THES
A1  - Wunderling, Nico
T1  - Nichtlineare Dynamiken und Interaktionen von Kippelementen im Erdsystem
T1  - Nonlinear dynamics and interactions of tipping elements in the Earth system
N2  - With ongoing anthropogenic global warming, some of the most vulnerable components of the Earth system might become unstable and undergo a critical transition. These subsystems are the so-called tipping elements. They are believed to exhibit threshold behaviour and would, if triggered, result in severe consequences for the biosphere and human societies. Furthermore, it has been shown that climate tipping elements are not isolated entities, but interact across the entire Earth system. Therefore, this thesis aims at mapping out the potential for tipping events and feedbacks in the Earth system mainly by the use of complex dynamical systems and network science approaches, but partially also by more detailed process-based models of the Earth system.

In the first part of this thesis, the theoretical foundations are laid by the investigation of networks of interacting tipping elements. For this purpose, the conditions for the emergence of global cascades are analysed against the structure of paradigmatic network types such as Erdös-Rényi, Barabási-Albert, Watts-Strogatz and explicitly spatially embedded networks. Furthermore, micro-scale structures are detected that are decisive for the transition of local to global cascades. These so-called motifs link the micro- to the macro-scale in the network of tipping elements. Alongside a model description paper, all these results are entered into the Python software package PyCascades, which is publicly available on github.

In the second part of this dissertation, the tipping element framework is first applied to components of the Earth system such as the cryosphere and to parts of the biosphere. Afterwards it is applied to a set of interacting climate tipping elements on a global scale. Using the Earth system Model of Intermediate Complexity (EMIC) CLIMBER-2, the temperature feedbacks are quantified, which would arise if some of the large cryosphere elements disintegrate over a long span of time. The cryosphere components that are investigated are the Arctic summer sea ice, the mountain glaciers, the Greenland and the West Antarctic Ice Sheets. The committed temperature increase, in case the ice masses disintegrate, is on the order of an additional half a degree on a global average (0.39-0.46 °C), while local to regional additional temperature increases can exceed 5 °C. This means that, once tipping has begun, additional reinforcing feedbacks are able to increase global warming and with that the risk of further tipping events.

This is also the case in the Amazon rainforest, whose parts are dependent on each other via the so-called moisture-recycling feedback. In this thesis, the importance of drought-induced tipping events in the Amazon rainforest is investigated in detail. Despite the Amazon rainforest is assumed to be adapted to past environmental conditions, it is found that tipping events sharply increase if the drought conditions become too intense in a too short amount of time, outpacing the adaptive capacity of the Amazon rainforest. In these cases, the frequency of tipping cascades also increases to 50% (or above) of all tipping events. In the model that was developed in this study, the southeastern region of the Amazon basin is hit hardest by the simulated drought patterns. This is also the region that already nowadays suffers a lot from extensive human-induced changes due to large-scale deforestation, cattle ranching or infrastructure projects.

Moreover, on the larger Earth system wide scale, a network of conceptualised climate tipping elements is constructed in this dissertation making use of a large literature review, expert knowledge and topological properties of the tipping elements. In global warming scenarios, tipping cascades are detected even under modest scenarios of climate change, limiting global warming to 2 °C above pre-industrial levels. In addition, the structural roles of the climate tipping elements in the network are revealed. While the large ice sheets on Greenland and Antarctica are the initiators of tipping cascades, the Atlantic Meridional Overturning Circulation (AMOC) acts as the transmitter of cascades. Furthermore, in our conceptual climate tipping element model, it is found that the ice sheets are of particular importance for the stability of the entire system of investigated climate tipping elements.

In the last part of this thesis, the results from the temperature feedback study with the EMIC CLIMBER-2 are combined with the conceptual model of climate tipping elements. There, it is observed that the likelihood of further tipping events slightly increases due to the temperature feedbacks even if no further CO$_2$ would be added to the atmosphere.

Although the developed network model is of conceptual nature, it is possible with this work for the first time to quantify the risk of tipping events between interacting components of the Earth system under global warming scenarios, by allowing for dynamic temperature feedbacks at the same time.
N2  - Bei fortdauerndem anthropogenem Klimawandel, könnten einige der vulnerabelsten Komponenten des Erdsystem instabil werden und in einen anderen Zustand übergehen. Diese Komponenten des Erdsystems sind die sogenannten Kippelemente. Bei ihnen wird angenommen, dass sie einen Kipppunkt besitzen ab dem sie in einen qualitativ anderen Zustand übergehen können. Sollte das passieren, hätte das schwerwiegende Konsequenzen für die Biosphäre und menschliche Gesellschaften. Des Weiteren ist gezeigt worden, dass Kippelemente keine isolierte Reigionen oder Prozesse sind, sondern über das gesamte Erdsystem hinweg interagieren. Das Ziel dieser Arbeit ist es daher, die Wahrscheinlichkeit für Kippereignisse sowie deren Feedbacks im Erdsystem zu quantifizieren. Zu diesem Zweck kommen vor allem Frameworks aus der Wissenschaft komplexer Systeme und Netzwerke zum Einsatz. Für einige Teilaspekte dieser Arbeit wird aber auch ein detaillierteres und prozessbasierteres Erdsystemmodell verwendet.

Im ersten Teil dieser Arbeit werden die theoretischen Grundlagen gelegt, indem komplexe Netzwerke bestehend aus interagierenden Kippelementen untersucht werden. Hier werden Voraussetzungen für das Auftreten globaler Kippkaskaden anhand der Struktur paradigmatischer Netzwerktypen analysiert. Diese Typen sind Netzwerke wie Erdös-Rényi, Barabási-Albert, Watts-Strogatz Netzwerke oder auch explizit räumlich eingebettete Netzwerke. Darüber hinaus sind bestimmte Mikrostrukturen in Netzwerken dafür entscheidend, ob sich eine lokale Kaskaden auf das globale Netzwerk ausbreiten kann. Diese Strukturen sind das Bindeglied zwischen der Mikro- und der Makroebene des Netzwerks und werden Motive genannt. Zusammen mit einer Publikation zur Modellbeschreibung, werden alle diese Ergebnisse im Python-Softwarepaket PyCascades veröffentlicht, das auf github öffentlich verfügbar ist.

Im zweiten Teil dieser Dissertation wird das Kippelementframework zunächst auf Kompenenten des Erdsystems angewendet wie der Kryosphäre und Teilen der Biosphäre, und danach auf globaler Skala für interagierende Klimakippelemente. In einem ersten Schritt werden mit dem Erdsystemmodell mittlerer Komplexität CLIMBER-2 die Temperaturfeedbacks ermittelt, die entstehen würden, wenn große Gebiete der Kryosphäre auf lange Sicht eisfrei werden. In dieser Berechnung werden das arktische Sommermeereis, die Gebirgsgletscher, der grönländische und der westantarktische Eisschild berücksichtigt. Die quantifizierte Temperaturerhöhung liegt in der Größenordnung von einem halben Grad zusätzlicher globaler Erwärmung (0.39--0.46°C). Lokale bis regionale Temperaturerhöhungen können allerdings 5°C übersteigen. Wenn also das Kippen einiger Elemente begonnen hat, bedeutet dieses Ergebnis, dass Temperaturfeedbacks in der Lage sind, das Risiko weiterer Kippereignisse zu erhöhen.

Dies ist auch der Fall im Amazonasregenwald, dessen Unterregionen über den sogenannten Feuchtig-keits-Recycling-Feedback miteinander in Beziehung stehen und voneinander abhängen. In dieser Dissertation wird die Bedeutung von Kippereignissen im Detail untersucht, die aufgrund von Dürreperioden zustande kommen. Obwohl man davon ausgehen kann, dass der Regenwald sich an zurückliegende und gegenwärtige Klimabedingungen angepasst hat, kann festgestellt werden, dass die Häu-figkeit von Kippereignissen stark zunimmt, wenn die jeweilige Trockenperiode eine gewisse Intensität übersteigt und damit die Anpassungsfähigkeit des Amazonasregenwalds überschritten wird. In solchen Fällen steigt auch die Häufigkeit von Kippkaskaden unter allen Kippereignissen auf 50% (und mehr) an. In dem Modell, das in dieser Studie entwickelt wurde, zeigt sich, dass der Südosten des Amazonasbeckens am stärksten von den simulierten Trockenheitsmustern betroffen ist. Das ist gleichzeitig die Region, die bereits heute stark unter anthropogener Veränderung leidet, unter anderem aufgrund von großflächiger Abholzung, Viehzucht oder Infrastrukturprojekten.

Zudem wird in dieser Dissertation auf der größeren, erdsystemweiten Skala ein Netzwerk konzeptionalisierter Klimakippelemente aufgebaut. Zu diesem Zweck wird eine umfangreiche Literaturrecherche durchgeführt, die zusammen mit Expertenwissen und den topologischen Eigenschaften der Kippelemente in die Studien mit einfließt. In Klimawandelszenarien können dann Kippkaskaden beobachtet werden, selbst wenn die globale Erderwärmung auf 2°C über dem vorindustriellen Niveau begrenzt werden kann. Außerdem werden die strukturellen Rollen der Klimakippelemente im Netzwerk ermittelt. Während die großen Eisschilde auf Grönland und der Westantarktis viele Kippkaskaden initiieren, ist die Atlantische Umwälzzirkulation für die Weitergabe vieler dieser Kaskaden verantwortlich. In unserem konzeptionellen Modell für Klimakippelemente wird darüber hinaus festgestellt, dass die Eisschilde von besonderer Bedeutung für die Stabilität des Gesamtsystems sind.

Im letzen Teil dieser Dissertation werden die Ergebnisse der Feedbackstudie (CLIMBER-2-Studie) zusammengebracht mit dem konzeptionellen Klimakippelementmodell. Dabei zeigt sich, dass die Wahrscheinlichkeit zusätzlicher Kippereignisse aufgrund der berücksichtigten Temperaturfeedbacks auch ohne das Zuführen eines zusätzlichen CO2-Eintrags in die Atmosphäre leicht ansteigt.

Trotz der konzeptionellen Natur des entwickelten Netzwerkmodells, ist es mit dieser Arbeit erstmals möglich eine Risikoabschätzung über das Auftreten von Kippkaskaden im Erdsystem vorzunehmen. Darüber hinaus können, unter der Annahme globaler Erwärmungsszenarien, auch dynamische Temperaturfeedbacks berücksichtigt werden.
KW  - tipping element
KW  - nonlinear dynamics
KW  - tipping cascade
KW  - climate change
KW  - complex networks
KW  - Klimawandel
KW  - komplexe Netzwerke
KW  - nichtlineare Dynamiken
KW  - Kippkaskade
KW  - Kippelement
Y1  - 2021
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-525140
ER  -