TY  - THES
A1  - Liepertz, Sven Christian
T1  - Zusammenhang zwischen dem Professionswissen von Physiklehrkräften, dem sachstrukturellen Angebot des Unterrichts und der Schülerleistung
T2  - Studien zum Physik- und Chemielernen ; 224
Y1  - 2017
SN  - 978-3-8325-4480-5
PB  - Logos
CY  - Berlin
ER  - 
TY  - JOUR
A1  - Sanjurjo-Ferrrin, G.
A1  - Torrejon, J. M.
A1  - Postnov, K.
A1  - Oskinova, Lida
A1  - Rodes-Roca, J. J.
A1  - Bernabeu, Guillermo
T1  - XMM-Newton spectroscopy of the accreting magnetar candidate 4U0114+65
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Methods. We analysed the energy-resolved light curve and the time-resolved X-ray spectra provided by the EPIC cameras on board XMM-Newton. We also analysed the first high-resolution spectrum of this source provided by the Reflection Grating Spectrometer. Results. An X-ray pulse of 9350 +/- 160 s was measured. Comparison with previous measurements confirms the secular spin up of this source. We successfully fit the pulse-phase-resolved spectra with Comptonisation models. These models imply a very small (r similar to 3 km) and hot (kT similar to 2-3 keV) emitting region and therefore point to a hot spot over the neutron star (NS) surface as the most reliable explanation for the X-ray pulse. The long NS spin period, the spin-up rate, and persistent X-ray emission can be explained within the theory of quasi-spherical settling accretion, which may indicate that the magnetic field is in the magnetar range. Thus, 4U0114+65 could be a wind-accreting magnetar. We also observed two episodes of low luminosity. The first was only observed in the low-energy light curve and can be explained as an absorption by a large over-dense structure in the wind of the B1 supergiant donor. The second episode, which was deeper and affected all energies, may be due to temporal cessation of accretion onto one magnetic pole caused by non-spherical matter capture from the structured stellar wind. The light curve displays two types of dips that are clearly seen during the high-flux intervals. The short dips, with durations of tens of seconds, are produced through absorption by wind clumps. The long dips, in turn, seem to be associated with the rarefied interclump medium. From the analysis of the X-ray spectra, we found evidence of emission lines in the X-ray photoionised wind of the B1Ia donor. The Fe K alpha line was found to be highly variable and much weaker than in other X-ray binaries with supergiant donors. The degree of wind clumping, measured through the covering fraction, was found to be much lower than in supergiant donor stars with earlier spectral types. Conclusions. The XMM-Newton spectroscopy provided further support for the magnetar nature of the neutron star in 4U0114+65. The light curve presents dips that can be associated with clumps and the interclump medium in the stellar wind of the mass donor.
KW  - X-rays: binaries
KW  - stars: winds, outflows
KW  - pulsars: individual: 4U0114+65
Y1  - 2017
U6  - https://doi.org/10.1051/0004-6361/201630119
SN  - 1432-0746
VL  - 606
SP  - 4039
EP  - 4042
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Miedema, P. S.
A1  - Mitzner, Rolf
A1  - Ganschow, S.
A1  - Föhlisch, Alexander
A1  - Beye, Martin
T1  - X-ray spectroscopy on the active ion in laser crystals
JF  - Physical chemistry, chemical physics : a journal of European Chemical Societies
N2  - The active ions in typical laser crystals were studied with Resonant Inelastic X-ray Scattering (RIXS) and Partial Fluorescence Yield X-ray Absorption (PFY-XAS) spectroscopies as solid state model systems for dilute active centers. We analyzed Ti3+ and Cr3+ in alpha-Al2O3:Ti3+ and LiCaAlF6:Cr3+, respectively. The comparison of experimental data with semi-empirical multiplet calculations provides insights into the electronic structure and shows how measured crystal field energies are related across different spectroscopies.
Y1  - 2017
U6  - https://doi.org/10.1039/c7cp03026f
SN  - 1463-9076
SN  - 1463-9084
VL  - 19
SP  - 21800
EP  - 21806
PB  - Royal Society of Chemistry
CY  - Cambridge
ER  - 
TY  - JOUR
A1  - De Becker, M.
A1  - del Valle, Maria Victoria
A1  - Romero, G. E.
A1  - Peri, C. S.
A1  - Benaglia, P.
T1  - X- ray study of bow shocks in runaway stars
JF  - Monthly notices of the Royal Astronomical Society
N2  - Massive runaway stars produce bow shocks through the interaction of their winds with the interstellar medium, with the prospect for particle acceleration by the shocks. These objects are consequently candidates for non-thermal emission. Our aim is to investigate the X-ray emission from these sources. We observed with XMM-Newton a sample of five bow shock runaways, which constitutes a significant improvement of the sample of bow shock runaways studied in X-rays so far. A careful analysis of the data did not reveal any X-ray emission related to the bow shocks. However, X-ray emission from the stars is detected, in agreement with the expected thermal emission from stellar winds. On the basis of background measurements we derive conservative upper limits between 0.3 and 10 keV on the bow shocks emission. Using a simple radiation model, these limits together with radio upper limits allow us to constrain some of the main physical quantities involved in the non-thermal emission processes, such as the magnetic field strength and the amount of incident infrared photons. The reasons likely responsible for the non-detection of non-thermal radiation are discussed. Finally, using energy budget arguments, we investigate the detectability of inverse Compton X-rays in a more extended sample of catalogued runaway star bow shocks. From our analysis we conclude that a clear identification of non-thermal X-rays from massive runaway bow shocks requires one order of magnitude (or higher) sensitivity improvement with respect to present observatories.
KW  - acceleration of particles
KW  - radiation mechanisms: non-thermal
KW  - stars: earlytype
KW  - X-rays: stars
Y1  - 2017
U6  - https://doi.org/10.1093/mnras/stx1826
SN  - 0035-8711
SN  - 1365-2966
VL  - 471
SP  - 4452
EP  - 4464
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Munoz, Melissa
A1  - Moffat, Anthony F. J.
A1  - Hill, Grant M.
A1  - Shenar, Tomer
A1  - Richardson, Noel D.
A1  - Pablo, Herbert
A1  - St-Louis, Nicole
A1  - Ramiaramanantsoa, Tahina
T1  - WR 148: identifying the companion of an extreme runaway massive binary
JF  - Monthly notices of the Royal Astronomical Society
N2  - WR 148 (HD 197406) is an extreme runaway system considered to be a potential candidate for a short-period (4.3173 d) rare WR + compact object binary. Provided with new high-resolution, high signal-to-noise spectra from the Keck observatory, we determine the orbital parameters for both the primary WR and the secondary, yielding respective projected orbital velocity amplitudes of 88.1 ± 3.8 km s−1 and 79.2 ± 3.1 km s−1 and implying a mass ratio of 1.1 ± 0.1. We then apply the shift-and-add technique to disentangle the spectra and obtain spectra compatible with a WN7ha and an O4-6 star. Considering an orbital inclination of ∼67°, derived from previous polarimetry observations, the system's total mass would be a mere 2–3M⊙⁠, an unprecedented result for a putative massive binary system. However, a system comprising a 37M⊙ secondary (typical mass of an O5V star) and a 33M⊙ primary (given the mass ratio) would infer an inclination of ∼18°. We therefore reconsider the previous methods of deriving the orbital inclination based on time-dependent polarimetry and photometry. While the polarimetric results are inconclusive requiring better data, the photometric results favour low inclinations. Finally, we compute WR 148’s space velocity and retrace the runaway's trajectory back to the Galactic plane (GP). With an ejection velocity of 198 ± 27 km s−1 and a travel time of 4.7 ± 0.8 Myr to reach its current location, WR 148 was most likely ejected via dynamical interactions in a young cluster.
KW  - binaries: spectroscopic
KW  - stars: individual: WR 148
KW  - stars: kinematics and dynamics
KW  - stars: mass-loss
KW  - stars: winds, outflows
KW  - stars: Wolf-Rayet
Y1  - 2017
U6  - https://doi.org/10.1093/mnras/stw2283
SN  - 0035-8711
SN  - 1365-2966
VL  - 467
SP  - 3105
EP  - 3121
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Leussu, R.
A1  - Usoskin, IIlya G.
A1  - Valliappan, Senthamizh Pavai
A1  - Diercke, Andrea
A1  - Arlt, Rainer
A1  - Denker, Carsten
A1  - Mursula, K.
T1  - Wings of the butterfly
BT  - sunspot groups for 1826-2015
JF  - Astronomy and astrophysics : an international weekly journal
N2  - The spatio-temporal evolution of sunspot activity, the so-called Maunder butterfly diagram, has been continously available since 1874 using data from the Royal Greenwich Observatory, extended by SOON network data after 1976. Here we present a new extended butterfly diagram of sunspot group occurrence since 1826, using the recently digitized data from Schwabe (1826-1867) and Sporer (1866-1880). The wings of the diagram are separated using a recently developed method based on an analysis of long gaps in sunspot group occurrence in different latitude bands. We define characteristic latitudes, corresponding to the start, end, and the largest extent of the wings (the F, L, and H latitudes). The H latitudes (30 degrees-45 degrees) are highly significantly correlated with the strength of the wings (quantified by the total sum of the monthly numbers of sunspot groups). The F latitudes (20 degrees-30 degrees) depict a weak tendency, especially in the southern hemisphere, to follow the wing strength. The L latitudes (2 degrees-10 degrees) show no clear relation to the wing strength. Overall, stronger cycle wings tend to start at higher latitudes and have a greater wing extent. A strong (5-6)-cycle periodic oscillation is found in the start and end times of the wings and in the overlap and gaps between successive wings of one hemisphere. While the average wing overlap is zero in the southern hemisphere, it is two to three months in the north. A marginally significant oscillation of about ten solar cycles is found in the asymmetry of the L latitudes. The new long database of butterfly wings provides new observational constraints to solar dynamo models that discuss the spatio-temporal distribution of sunspot occurrence over the solar cycle and longer.
KW  - Sun: activity
KW  - sunspots
KW  - history and philosophy of astronomy
Y1  - 2017
U6  - https://doi.org/10.1051/0004-6361/201629533
SN  - 1432-0746
VL  - 599
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - THES
A1  - Kayser, Markus
T1  - Wechselwirkung der atmosphärischen Grenzschicht mit synoptisch–skaligen Prozessen während der N-ICE2015 Kampagne
N2  - Die Arktis erwärmt sich schneller als der Rest der Erde. Die Auswirkungen manifestieren sich unter Anderem in einer verstärkten Erwärmung der arktischen Grenzschicht. Diese Arbeit befasst sich mit Wechselwirkungen zwischen synoptischen Zyklonen und der arktischen Atmosphäre auf lokalen bis überregionalen Skalen. Ausgangspunkt dafür sind Messdaten und Modellsimulationen für den Zeitraum der N-ICE2015 Expedition, die von Anfang Januar bis Ende Juni 2015 im arktischen Nordatlantiksektor stattgefunden hat.
Anhand von Radiosondenmessungen lassen sich Auswirkungen von synoptischen Zyklonen am deutlichsten im Winter erkennen, da sie durch die Advektion warmer und feuchter Luftmassen in die Arktis den Zustand der Atmosphäre von einem strahlungs-klaren in einen strahlungs-opaken ändern. Obwohl dieser scharfe Kontrast nur im Winter existiert, zeigt die Analyse, dass der integrierte Wasserdampf als Indikator für die Advektion von Luftmassen aus niedrigen Breiten in die Arktis auch im Frühjahr geeignet ist. Neben der Advektion von Luftmassen wird der Einfluss der Zyklonen auf die statische Stabilität charakterisiert. Beim Vergleich der N-ICE2015 Beobachtungen mit der SHEBA Kampagne (1997/1998), die über dickerem Eis stattfand, finden sich trotz der unterschiedlichen Meereisregime Ähnlichkeiten in der statischen Stabilität der Atmosphäre. Die beobachteten Differenzen in der Stabilität lassen sich auf Unterschiede in der synoptischen Aktivität zurückführen. Dies lässt vermuten, dass die dünnere Eisdecke auf saisonalen Zeitskalen nur einen geringen Einfluss auf die thermodynamische Struktur der arktischen Troposphäre besitzt, solange eine dicke Schneeschicht sie bedeckt. Ein weiterer Vergleich mit den parallel zur N-ICE2015 Kampagne gestarteten Radiosonden der AWIPEV Station in Ny-Åesund, Spitzbergen, macht deutlich, dass die synoptischen Zyklonen oberhalb der Orographie auf saisonalen Zeitskalen das Wettergeschehen bestimmen.
Des Weiteren werden für Februar 2015 die Auswirkungen von in der Vertikalen variiertem Nudging auf die Entwicklung der Zyklonen am Beispiel des hydrostatischen regionalen Klimamodells HIRHAM5 untersucht. Es zeigt sich, dass die Unterschiede zwischen den acht Modellsimulationen mit abnehmender Anzahl der genudgten Level zunehmen. Die größten Differenzen resultieren vornehmlich aus dem zeitlichen Versatz der Entwicklung synoptischer Zyklonen. Zur Korrektur des Zeitversatzes der Zykloneninitiierung genügt es bereits, Nudging in den unterstem 250 m der Troposphäre anzuwenden. Daneben findet sich zwischen den genudgten HIRHAM5-Simulation und den in situ Messungen der gleiche positive Temperaturbias, den auch ERA-Interim besitzt. Das freie HIRHAM hingegen reproduziert das positive Ende der N-ICE2015 Temperaturverteilung gut, besitzt aber einen starken negativen Bias, der sehr wahrscheinlich aus einer Unterschätzung des Feuchtegehalts resultiert. An Beispiel einer Zyklone wird gezeigt, dass Nudging Einfluss auf die Lage der Höhentiefs besitzt, die ihrerseits die Zyklonenentwicklung am Boden beeinflussen. Im Weiteren wird mittels eines für kleine Ensemblegrößen geeigneten Varianzmaßes eine statistische Einschätzung der Wirkung des Nudgings auf die Vertikale getroffen. Es wird festgestellt, dass die Ähnlichkeit der Modellsimulationen in der unteren Troposphäre generell höher ist als darüber und in 500 hPa ein lokales Minimum besitzt.
Im letzten Teil der Analyse wird die Wechselwirkung der oberen und unteren Stratosphäre anhand zuvor betrachteter Zyklonen mit Daten der ERA-Interim Reanalyse untersucht. Lage und Ausrichtung des Polarwirbels erzeugten ab Anfang Februar 2015 eine ungewöhnlich große Meridionalkomponente des Tropopausenjets, die Zugbahnen in die zentrale Arktis begünstigte. Am Beispiel einer Zyklone wird die Übereinstimmung der synoptischen Entwicklung mit den theoretischen Annahmen über den abwärts gerichteten Einfluss der Stratosphäre auf die Troposphäre hervorgehoben. Dabei spielt die nicht-lineare Wechselwirkung zwischen der Orographie Grönlands, einer Intrusion stratosphärischer Luft in die Troposphäre sowie einer in Richtung Arktis propagierender Rossby-Welle eine tragende Rolle. Als Indikator dieser Wechselwirkung werden horizontale Signaturen aus abwechselnd aufsteigender und absinkender Luft innerhalb der Troposphäre identifiziert.
N2  - The Arctic warms faster than the rest of the earth. The causes and effects of this arctic amplification are manifested in the arctic atmosphere, especially in the atmospheric boundary layer, which plays a key role in the exchange processes of the atmosphere, ocean and sea ice. This work highlights the importance of synoptic cyclones in the Arctic North Atlantic region. For this purpose, the influence of synoptic cyclones on the Arctic boundary layer as well as their interactions with different regions within the Arctic atmosphere on local to supraregional scales is investigated. The starting point for this are measurement data and model simulations for the period of the NICE2015 expedition, which took place in the Arctic North Atlantic region from early January to late June 2015.
On the basis of radiosonde measurements, the effects of synoptic cyclones are most noticeable in the winter because, by the advection of warm and humid air masses into the Arctic, the condition of the atmosphere changes from a radiative clear to opaquely cloudy. Although this sharp contrast only exists in winter, the analysis shows that integrated water vapor is an indicator for the advection of air masses from low latitudes into the Arctic even in the spring. In addition to the advection of air masses, the influence of cyclones on static stability is characterized. Comparing the N-ICE2015 observations with the SHEBA campaign (1997/1998), which took place over thicker ice, similarities are found in the static stability of the atmosphere despite the different sea ice regimes. The observed differences in stability can be attributed to differences in synoptic activity. A further comparison with the radiosondes of the AWIPEV station in Ny-Åesund, Spitzbergen, which were launched parallel to the N-ICE2015 campaign, shows that synoptic cyclones determine the course of the winter months. In addition, the effects of vertically-varying nudging on the development of cyclones is examined for February 2015 using the hydrostatic regional climate model HIRHAM5. It is shown that the differences between the eight model simulations are increasing with decreasing number of nudged levels. The greatest differences are mainly due to the temporal offset of the development of synoptic cyclones. To correct the time offset of the cyclone initiation, it is sufficient to use nudging in the lowest troposphere. The free HIRHAM reproduces the positive end of the N-ICE2015 temperature distribution well, but has a strong negative bias which most likely results from an under-estimation of the moisture content. An example of a cyclone shows that nudging has an influence on the position of the high altitude lows, which in turn influences cyclone development on the ground. Furthermore, a statistical estimate of the effect of nudging on the vertical is made by means of a variance measure suitable for small ensemble sizes. It is found that the similarity of model simulations in the lower troposphere is generally higher than above and has a local minimum in 500 hPa.
In the last part of the analysis, the interaction of the upper troposphere and the lower stratosphere is investigated with data from the ERA interim reanalysis using previously examined cyclones. The position and orientation of the polar vortex produced an unusually large meridional component of the tropopause jets, which favored passage of low pressure systems into the central Arctic from the beginning of February 2015 onwards. Using a cyclone as an example, the synoptic development is compared with the theoretical assumptions about the downward impact of the stratosphere on the troposphere. The non-linear interaction between Greenland’s orography, an intrusion of stratospheric air into the troposphere, and a Rossby wave propagating in the direction of the Arctic play a key role in the selected time frame. As an indicator of this interaction, horizontal signatures are identified from alternately ascending and descending air within the troposphere.
KW  - arktische Grenzschicht
KW  - Arctic boundary layer
KW  - synoptische Zyklone
KW  - synoptic cyclones
KW  - thermodynamische Struktur
KW  - thermodynamic structure
KW  - regional climate simulations
KW  - regionale Klimasimulationen
KW  - nudging
Y1  - 2017
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-411124
ER  - 
TY  - JOUR
A1  - Allen, C.
A1  - Archambault, S.
A1  - Archer, A.
A1  - Benbow, W.
A1  - Bird, R.
A1  - Bourbeau, E.
A1  - Brose, Robert
A1  - Buchovecky, M.
A1  - Buckley, J. H.
A1  - Bugaev, V.
A1  - Cardenzana, J. V.
A1  - Cerruti, M.
A1  - Chen, Xuhui
A1  - Christiansen, J. L.
A1  - Connolly, M. P.
A1  - Cui, W.
A1  - Daniel, M. K.
A1  - Eisch, J. D.
A1  - Falcone, Abe
A1  - Feng, Q.
A1  - Fernandez-Alonso, M.
A1  - Finley, J. P.
A1  - Fleischhack, H.
A1  - Flinders, A.
A1  - Fortson, L.
A1  - Furniss, A.
A1  - Gillanders, G. H.
A1  - Griffin, S.
A1  - Grube, J.
A1  - Huetten, M.
A1  - Hakansson, N.
A1  - Hanna, D.
A1  - Hervet, O.
A1  - Holder, J.
A1  - Hughes, G.
A1  - Humensky, T. B.
A1  - Johnson, C. A.
A1  - Kaaret, P.
A1  - Kar, P.
A1  - Kelley-Hoskins, N.
A1  - Kertzman, M.
A1  - Kieda, D.
A1  - Krause, M.
A1  - Krennrich, F.
A1  - Kumar, S.
A1  - Lang, M. J.
A1  - Maier, G.
A1  - McArthur, S.
A1  - McCann, A.
A1  - Meagher, K.
A1  - Moriarty, P.
A1  - Mukherjee, R.
A1  - Nguyen, T.
A1  - Nieto, D.
A1  - Ong, R. A.
A1  - Otte, A. N.
A1  - Park, N.
A1  - Petrashyk, A.
A1  - Pichel, A.
A1  - Pohl, Martin
A1  - Popkow, A.
A1  - Pueschel, Elisa
A1  - Quinn, J.
A1  - Ragan, K.
A1  - Reynolds, P. T.
A1  - Richards, G. T.
A1  - Roache, E.
A1  - Rovero, A. C.
A1  - Rulten, C.
A1  - Sadeh, I.
A1  - Santander, Marcos
A1  - Sembroski, G. H.
A1  - Shahinyan, K.
A1  - Telezhinsky, Igor O.
A1  - Tucci, J. V.
A1  - Tyler, J.
A1  - Wakely, S. P.
A1  - Weinstein, A.
A1  - Wilhelm, Alina
A1  - Williams, D. A.
T1  - Very-High-Energy gamma-Ray Observations of the Blazar 1ES 2344+514 with VERITAS
JF  - Monthly notices of the Royal Astronomical Society
N2  - We present very-high-energy gamma-ray observations of the BL Lac object 1ES 2344+514 taken by the Very Energetic Radiation Imaging Telescope Array System between 2007 and 2015. 1ES 2344+514 is detected with a statistical significance above the background of 20.8 sigma in 47.2 h (livetime) of observations, making this the most comprehensive very-high-energy study of 1ES 2344+514 to date. Using these observations, the temporal properties of 1ES 2344+514 are studied on short and long times-scales. We fit a constant-flux model to nightly and seasonally binned light curves and apply a fractional variability test to determine the stability of the source on different time-scales. We reject the constant-flux model for the 2007-2008 and 2014-2015 nightly binned light curves and for the long-term seasonally binned light curve at the > 3 sigma level. The spectra of the time-averaged emission before and after correction for attenuation by the extragalactic background light are obtained. The observed time-averaged spectrum above 200 GeV is satisfactorily fitted (x(2)/NDF = 7.89/6) by a power-law function with an index Gamma = 2.46 +/- 0.06(stat) +/- 0.20(sys) and extends to at least 8 TeV. The extragalactic-backgroundlight-deabsorbed spectrum is adequately fit (x(2)/NDF = 6.73/6) by a power-law function with an index Gamma = 2.15 +/- 0.06(stat) +/- 0.20(sys) while an F-test indicates that the power law with an exponential cut-off function provides a marginally better fit (x(2)/NDF = 2.56/5) at the 2.1 sigma level. The source location is found to be consistent with the published radio location and its spatial extent is consistent with a point source.
KW  - astroparticle physics
KW  - BL Lacertae objects: individual: 1ES 2344+514=VERJ2347+517
KW  - gamma-rays: galaxies
Y1  - 2017
U6  - https://doi.org/10.1093/mnras/stx1756
SN  - 0035-8711
SN  - 1365-2966
VL  - 471
SP  - 2117
EP  - 2123
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Kayser, Markus
A1  - Maturilli, Marion
A1  - Graham, Robert M.
A1  - Hudson, Stephen R.
A1  - Rinke, Annette
A1  - Cohen, Lana
A1  - Kim, Joo-Hong
A1  - Park, Sang-Jong
A1  - Moon, Woosok
A1  - Granskog, Mats A.
T1  - Vertical thermodynamic structure of the troposphere during the Norwegian young sea ICE expedition (N-ICE2015)
JF  - Journal of geophysical research-atmosheres
N2  - The Norwegian young sea ICE (N-ICE2015) expedition was designed to investigate the atmosphere-snow-ice-ocean interactions in the young and thin sea ice regime north of Svalbard. Radiosondes were launched twice daily during the expedition from January to June 2015. Here we use these upper air measurements to study the multiple cyclonic events observed during N-ICE2015 with respect to changes in the vertical thermodynamic structure, moisture content, and boundary layer characteristics. We provide statistics of temperature inversion characteristics, static stability, and boundary layer extent. During winter, when radiative cooling is most effective, we find the strongest impact of synoptic cyclones. Changes to thermodynamic characteristics of the boundary layer are associated with transitions between the radiatively "clear" and "opaque" atmospheric states. In spring, radiative fluxes warm the surface leading to lifted temperature inversions and a statically unstable boundary layer. Further, we compare the N-ICE2015 static stability distributions to corresponding profiles from ERA-Interim reanalysis, from the closest land station in the Arctic North Atlantic sector, Ny-Alesund, and to soundings from the SHEBA expedition (1997/1998). We find similar stability characteristics for N-ICE2015 and SHEBA throughout the troposphere, despite differences in location, sea ice thickness, and snow cover. For Ny-Alesund, we observe similar characteristics above 1000 m, while the topography and ice-free fjord surrounding Ny-Alesund generate great differences below. The long-term radiosonde record (1993-2014) from Ny-Alesund indicates that during the N-ICE2015 spring period, temperatures were close to the climatological mean, while the lowest 3000 m were 1-3 degrees C warmer than the climatology during winter. Plain Language Summary The Norwegian young sea ICE (N-ICE2015) expedition was designed to investigate the atmosphere-snow-ice-ocean interactions in the young and thin sea ice regime north of Svalbard. Radiosondes were launched twice daily during the expedition from January to June 2015. Here we use these upper air measurements to study the multiple cyclonic events observed during N-ICE2015 with respect to changes in the vertical thermodynamic structure, moisture content, and the atmospheric boundary layer characteristics. During winter, we find the strongest impact of synoptic cyclones, which transport warm and moist air into the cold and dry Arctic atmosphere. In spring, incoming solar radiation warms the surface. This leads to very different thermodynamic conditions and higher moisture content, which reduces the contrast between stormy and calm periods. Further, we compare the N-ICE2015 measurements to corresponding profiles from ERA-Interim reanalysis, from the closest land station in the Arctic North Atlantic sector, Ny-Alesund, and to soundings from the SHEBA expedition (1997/1998). We find similar stability characteristics for N-ICE2015 and SHEBA throughout the troposphere, despite differences in location, sea ice thickness, and snow cover. The comparisons highlight the value of the N-ICE2015 observation and show the importance of winter time observations in the Arctic North Atlantic sector.
Y1  - 2017
U6  - https://doi.org/10.1002/2016JD026089
SN  - 2169-897X
SN  - 2169-8996
VL  - 122
IS  - 20
SP  - 10855
EP  - 10872
PB  - American Geophysical Union
CY  - Washington
ER  - 
TY  - JOUR
A1  - Eckert, Sebastian
A1  - Niskanen, Johannes
A1  - Jay, Raphael Martin
A1  - Miedema, Piter S.
A1  - Fondell, Mattis
A1  - Kennedy, Brian
A1  - Quevedo, Wilson
A1  - Iannuzzi, Marcella
A1  - Föhlisch, Alexander
T1  - Valence orbitals and local bond dynamics around N atoms of histidine under X-ray irradiation
JF  - Physical chemistry, chemical physics : a journal of European Chemical Societies
N2  - The valence orbitals of aqueous histidine under basic, neutral and acidic conditions and their X-ray induced transformations have been monitored through N 1s resonant inelastic X-ray scattering. Using density functional ab initio molecular dynamics simulations in the core-hole state within the Z + 1 approximation, core-excitation-induced molecular transformations are quantified. Spectroscopic evidence for a highly directional X-ray-induced local N-H dissociation within the scattering duration is presented for acidic histidine. Our report demonstrates a protonation-state and chemical-environment dependent propensity for a molecular dissociation, which is induced by the absorption of high energy photons. This case study indicates that structural deformations in biomolecules under exposure to ionizing radiation, yielding possible alteration or loss of function, is highly dependent on the physiological state of the molecule upon irradiation.
Y1  - 2017
U6  - https://doi.org/10.1039/c7cp05713j
SN  - 1463-9076
SN  - 1463-9084
VL  - 19
SP  - 32091
EP  - 32098
PB  - Royal Society of Chemistry
CY  - Cambridge
ER  - 
TY  - GEN
A1  - Eckert, Sebastian
A1  - Norell, Jesper
A1  - Miedema, Piter S.
A1  - Beye, Martin
A1  - Fondell, Mattis
A1  - Quevedo, Wilson
A1  - Kennedy, Brian
A1  - Hantschmann, Markus
A1  - Pietzsch, Annette
A1  - van Kuiken, Benjamin E.
A1  - Ross, Matthew
A1  - Minitti, Michael P.
A1  - Moeller, Stefan P.
A1  - Schlotter, William F.
A1  - Khalil, Munira
A1  - Odelius, Michael
A1  - Föhlisch, Alexander
T1  - Untersuchung unabhängiger N‐H‐ und N‐C‐Bindungsverformungen auf ultrakurzen Zeitskalen mit resonanter inelastischer Röntgenstreuung
T2  - Postprints der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe
N2  - Die Femtosekundendynamik nach resonanten Photoanregungen mit optischen und Röntgenpulsen ermöglicht eine selektive Verformung von chemischen N‐H‐ und N‐C‐Bindungen in 2‐Thiopyridon in wässriger Lösung. Die Untersuchung der orbitalspezifischen elektronischen Struktur und ihrer Dynamik auf ultrakurzen Zeitskalen mit resonanter inelastischer Röntgenstreuung an der N1s‐Resonanz am Synchrotron und dem Freie‐Elektronen‐Laser LCLS in Kombination mit quantenchemischen Multikonfigurationsberechnungen erbringen den direkten Nachweis dieser kontrollierten photoinduzierten Molekülverformungen und ihrer ultrakurzen Zeitskala.
T3  - Zweitveröffentlichungen der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe - 1121 
KW  - Photochemie
KW  - Protonierung
KW  - RIXS (resonante inelastische Röntgenstreuung)
KW  - Selektiver Bindungsbruch
KW  - Stickstoff
Y1  - 2021
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-436688
SN  - 1866-8372
IS  - 1121
ER  - 
TY  - GEN
A1  - Hempel, Sabrina
A1  - Koseska, Aneta
A1  - Nikoloski, Zoran
A1  - Kurths, Jürgen
T1  - Unraveling gene regulatory networks from time-resolved gene expression data
BT  - a measures comparison study
N2  - Background: Inferring regulatory interactions between genes from transcriptomics time-resolved data, yielding reverse engineered gene regulatory networks, is of paramount importance to systems biology and bioinformatics studies. Accurate methods to address this problem can ultimately provide a deeper insight into the complexity, behavior, and functions of the underlying biological systems. However, the large number of interacting genes coupled with short and often noisy time-resolved read-outs of the system renders the reverse engineering a challenging task. Therefore, the development and assessment of methods which are computationally efficient, robust against noise, applicable to short time series data, and preferably capable of reconstructing the directionality of the regulatory interactions remains a pressing research problem with valuable applications.

Results: Here we perform the largest systematic analysis of a set of similarity measures and scoring schemes within the scope of the relevance network approach which are commonly used for gene regulatory network reconstruction from time series data. In addition, we define and analyze several novel measures and schemes which are particularly suitable for short transcriptomics time series. We also compare the considered 21 measures and 6 scoring schemes according to their ability to correctly reconstruct such networks from short time series data by calculating summary statistics based on the corresponding specificity and sensitivity. Our results demonstrate that rank and symbol based measures have the highest performance in inferring regulatory interactions. In addition, the proposed scoring scheme by asymmetric weighting has shown to be valuable in reducing the number of false positive interactions. On the other hand, Granger causality as well as information-theoretic measures, frequently used in inference of regulatory networks, show low performance on the short time series analyzed in this study.

Conclusions: Our study is intended to serve as a guide for choosing a particular combination of similarity measures and scoring schemes suitable for reconstruction of gene regulatory networks from short time series data. We show that further improvement of algorithms for reverse engineering can be obtained if one considers measures that are rooted in the study of symbolic dynamics or ranks, in contrast to the application of common similarity measures which do not consider the temporal character of the employed data. Moreover, we establish that the asymmetric weighting scoring scheme together with symbol based measures (for low noise level) and rank based measures (for high noise level) are the most suitable choices.
T3  - Zweitveröffentlichungen der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe - 371 
KW  - unferring cellular networks
KW  - mutual information
KW  - Escherichia-coli
KW  - cluster-analysis
KW  - series
KW  - algorithms
KW  - inference
KW  - models
KW  - recognition
KW  - variables
Y1  - 2017
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-400924
ER  - 
TY  - JOUR
A1  - Koc, Azize
A1  - Reinhardt, M.
A1  - von Reppert, Alexander
A1  - Roessle, Matthias
A1  - Leitenberger, Wolfram
A1  - Dumesnil, K.
A1  - Gaal, Peter
A1  - Zamponi, Flavio
A1  - Bargheer, Matias
T1  - Ultrafast x-ray diffraction thermometry measures the influence of spin excitations on the heat transport through nanolayers
JF  - Physical review : B, Condensed matter and materials physics
N2  - We investigate the heat transport through a rare earth multilayer system composed of yttrium (Y), dysprosium (Dy), and niobium (Nb) by ultrafast x-ray diffraction. This is an example of a complex heat flow problem on the nanoscale, where several different quasiparticles carry the heat and conserve a nonequilibrium for more than 10 ns. The Bragg peak positions of each layer represent layer-specific thermometers that measure the energy flow through the sample after excitation of the Y top layer with fs-laser pulses. In an experiment-based analytic solution to the nonequilibrium heat transport problem, we derive the individual contributions of the spins and the coupled electron-lattice system to the heat conduction. The full characterization of the spatiotemporal energy flow at different starting temperatures reveals that the spin excitations of antiferromagnetic Dy speed up the heat transport into the Dy layer at low temperatures, whereas the heat transport through this layer and further into the Y and Nb layers underneath is slowed down. The experimental findings are compared to the solution of the heat equation using macroscopic temperature-dependent material parameters without separation of spin and phonon contributions to the heat. We explain why the simulated energy density matches our experiment-based derivation of the heat transport, although the simulated thermoelastic strain in this simulation is not even in qualitative agreement.
Y1  - 2017
U6  - https://doi.org/10.1103/PhysRevB.96.014306
SN  - 2469-9950
SN  - 2469-9969
VL  - 96
PB  - American Physical Society
CY  - College Park
ER  - 
TY  - JOUR
A1  - Eckert, Sebastian
A1  - Norell, Jesper
A1  - Miedema, Piter S.
A1  - Beye, Martin
A1  - Fondell, Mattis
A1  - Quevedo, Wilson
A1  - Kennedy, Brian
A1  - Hantschmann, Markus
A1  - Pietzsch, Annette
A1  - Van Kuiken, Benjamin E.
A1  - Ross, Matthew
A1  - Minitti, Michael P.
A1  - Moeller, Stefan P.
A1  - Schlotter, William F.
A1  - Khalil, Munira
A1  - Odelius, Michael
A1  - Föhlisch, Alexander
T1  - Ultrafast Independent N-H and N-C Bond Deformation Investigated with Resonant Inelastic X-Ray Scattering
JF  - Angewandte Chemie : a journal of the Gesellschaft Deutscher Chemiker ; International edition
N2  - The femtosecond excited-state dynamics following resonant photoexcitation enable the selective deformation of N-H and N-C chemical bonds in 2-thiopyridone in aqueous solution with optical or X-ray pulses. In combination with multiconfigurational quantum-chemical calculations, the orbital-specific electronic structure and its ultrafast dynamics accessed with resonant inelastic X-ray scattering at the N 1s level using synchrotron radiation and the soft X-ray free-electron laser LCLS provide direct evidence for this controlled photoinduced molecular deformation and its ultrashort time-scale.
KW  - nitrogen
KW  - photochemistry
KW  - protonation
KW  - RIXS (resonant inelastic X-ray scattering)
KW  - selective bond cleavage
Y1  - 2017
U6  - https://doi.org/10.1002/anie.201700239
SN  - 1433-7851
SN  - 1521-3773
VL  - 56
SP  - 6088
EP  - 6092
PB  - Wiley-VCH
CY  - Weinheim
ER  - 
TY  - GEN
A1  - Eckert, Sebastian
A1  - Norell, Jesper
A1  - Miedema, Piter S.
A1  - Beye, Martin
A1  - Fondell, Mattis
A1  - Quevedo, Wilson
A1  - Kennedy, Brian
A1  - Hantschmann, Markus
A1  - Pietzsch, Annette
A1  - van Kuiken, Benjamin E.
A1  - Ross, Matthew
A1  - Minitti, Michael P.
A1  - Moeller, Stefan P.
A1  - Schlotter, William F.
A1  - Khalil, Munira
A1  - Odelius, Michael
A1  - Föhlisch, Alexander
T1  - Ultrafast Independent N-H and N-C Bond Deformation Investigated with Resonant Inelastic X-Ray Scattering
T2  - Postprints der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe
N2  - The femtosecond excited-state dynamics following resonant photoexcitation enable the selective deformation of N-H and N-C chemical bonds in 2-thiopyridone in aqueous solution with optical or X-ray pulses. In combination with multiconfigurational quantum-chemical calculations, the orbital-specific electronic structure and its ultrafast dynamics accessed with resonant inelastic X-ray scattering at the N 1s level using synchrotron radiation and the soft X-ray free-electron laser LCLS provide direct evidence for this controlled photoinduced molecular deformation and its ultrashort time-scale.
T3  - Zweitveröffentlichungen der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe - 1115 
KW  - nitrogen
KW  - photochemistry
KW  - protonation
KW  - RIXS (resonant inelastic X-ray scattering)
KW  - selective bond cleavage
Y1  - 2021
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-436873
SN  - 1866-8372
IS  - 1115
ER  - 
TY  - JOUR
A1  - Mor, Selene
A1  - Herzog, Marc
A1  - Golez, Denis
A1  - Werner, Philipp
A1  - Eckstein, Martin
A1  - Katayama, Naoyuki
A1  - Nohara, Minoru
A1  - Takagi, Hide
A1  - Mizokawa, Takashi
A1  - Monney, Claude
A1  - Staehler, Julia
T1  - Ultrafast Electronic Band Gap Control in an Excitonic Insulator
JF  - Physical review letters
N2  - We report on the nonequilibrium dynamics of the electronic structure of the layered semiconductor Ta2NiSe5 investigated by time-and angle-resolved photoelectron spectroscopy. We show that below the critical excitation density of F-C = 0.2 mJ cm(-2), the band gap narrows transiently, while it is enhanced above FC. Hartree-Fock calculations reveal that this effect can be explained by the presence of the low-temperature excitonic insulator phase of Ta2NiSe5, whose order parameter is connected to the gap size. This work demonstrates the ability to manipulate the band gap of Ta2NiSe5 with light on the femtosecond time scale.
Y1  - 2017
U6  - https://doi.org/10.1103/PhysRevLett.119.086401
SN  - 0031-9007
SN  - 1079-7114
VL  - 119
SP  - 11559
EP  - 11567
PB  - American Physical Society
CY  - College Park
ER  - 
TY  - JOUR
A1  - Thielemann-Kühn, Nele
A1  - Schick, Daniel
A1  - Pontius, Niko
A1  - Trabant, Christoph
A1  - Mitzner, Rolf
A1  - Holldack, Karsten
A1  - Zabel, Hartmut
A1  - Föhlisch, Alexander
A1  - Schuessler-Langeheine, Christian
T1  - Ultrafast and Energy-Efficient Quenching of Spin Order: Antiferromagnetism Beats Ferromagnetism
JF  - Physical review letters
N2  - By comparing femtosecond laser pulse induced ferro- and antiferromagnetic dynamics in one and the same material-metallic dysprosium-we show both to behave fundamentally different. Antiferromagnetic order is considerably faster and much more efficiently reduced by optical excitation than its ferromagnetic counterpart. We assign the fast and extremely efficient process in the antiferromagnet to an interatomic transfer of angular momentum within the spin system. Our findings imply that this angular momentum transfer channel is effective in other magnetic metals with nonparallel spin alignment. They also point out a possible route towards energy-efficient spin manipulation for magnetic devices.
Y1  - 2017
U6  - https://doi.org/10.1103/PhysRevLett.119.197202
SN  - 0031-9007
SN  - 1079-7114
VL  - 119
PB  - American Physical Society
CY  - College Park
ER  - 
TY  - GEN
A1  - Fraschetti, Federico
A1  - Pohl, Martin
T1  - Two-zone model for the broadband crab nebula spectrum
BT  - microscopic interpretation
T2  - The European physical journal : Web of Conferences : proceedings
N2  - We develop a simple two-zone interpretation of the broadband baseline Crab nebula spectrum between 10(-5) eV and similar to 100 TeV by using two distinct log-parabola energetic electrons distributions. We determine analytically the very-high energy photon spectrum as originated by inverse-Compton scattering of the far-infrared soft ambient photons within the nebula off a first population of electrons energized at the nebula termination shock. The broad and flat 200 GeV peak jointly observed by Fermi/LAT and MAGIC is naturally reproduced. The synchrotron radiation from a second energetic electron population explains the spectrum from the radio range up to similar to 10 keV. We infer from observations the energy dependence of the microscopic probability of remaining in proximity of the shock of the accelerating electrons.
Y1  - 2017
U6  - https://doi.org/10.1051/epjconf/201713602009
SN  - 2100-014X
VL  - 136
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Schubert, Marcel
A1  - Frisch, Johannes
A1  - Allard, Sybille
A1  - Preis, Eduard
A1  - Scherf, Ullrich
A1  - Koch, Norbert
A1  - Neher, Dieter
T1  - Tuning side chain and main chain order in a prototypical donor-acceptor copolymer
BT  - implications for optical, electronic, and photovoltaic characteristics
JF  - Elementary Processes in Organic Photovoltaics
N2  - The recent development of donor–acceptor copolymers has led to an enormous improvement in the performance of organic solar cells and organic field-effect transistors. Here we describe the synthesis, detailed characterisation, and application of a series of structurally modified copolymers to investigate fundamental structure–property relationships in this class of conjugated polymers. The interplay between chemical structure and optoelectronic properties is investigated. These are further correlated to the charge transport and solar cell performance, which allows us to link their chemical structure to the observed physical properties.
KW  - Aggregate states
KW  - All-polymer heterojunctions
KW  - Alternating copolymers
KW  - Ambipolar charge transport
KW  - Ambipolar materials
KW  - Backbone modifications
KW  - Bilayer solar cells
KW  - Charge separation
KW  - Conformational disorder
KW  - Crystalline phases
KW  - Donor-acceptor copolymers
KW  - Electron traps
KW  - Energetic disorder
KW  - Energy-level alignment
KW  - Fermi-level alignment
KW  - Fermi-level pinning
KW  - Interface dipole
KW  - Interlayer
KW  - Intrachain order
KW  - Intragap states
KW  - Microscopic morphology
KW  - Mobility imbalance
KW  - Mobility relaxation
KW  - Monte Carlo simulation
KW  - Multiple trapping model
KW  - Nonradiative recombination
KW  - OFET
KW  - Open-circuit voltage
KW  - Optoelectronic properties
KW  - Partially alternating copolymers
KW  - Photo-CELIV
KW  - Photocurrent
KW  - Photovoltaic gap
KW  - Polymer intermixing
KW  - Recombination losses
KW  - Spectral diffusion
KW  - Statistical copolymers
KW  - Stille-type cross-coupling
KW  - Structure-property relationships
KW  - Time-dependent mobility
KW  - Time-of-flight (TOF)
KW  - Transient photocurrent
KW  - Ultraviolet photoelectron spectroscopy
KW  - Vacuum-level alignment
KW  - X-ray photoelectron spectroscopy
Y1  - 2016
SN  - 978-3-319-28338-8
SN  - 978-3-319-28336-4
U6  - https://doi.org/10.1007/978-3-319-28338-8_10
SN  - 0065-3195
VL  - 272
SP  - 243
EP  - 265
PB  - Springer
CY  - Berlin
ER  - 
TY  - JOUR
A1  - Lechleitner, Franziska A.
A1  - Breitenbach, Sebastian Franz Martin
A1  - Rehfeld, Kira
A1  - Ridley, Harriet E.
A1  - Asmerom, Yemane
A1  - Prufer, Keith M.
A1  - Marwan, Norbert
A1  - Goswami, Bedartha
A1  - Kennett, Douglas J.
A1  - Aquino, Valorie V.
A1  - Polyak, Victor
A1  - Haug, Gerald H.
A1  - Eglinton, Timothy I.
A1  - Baldini, James U. L.
T1  - Tropical rainfall over the last two millennia: evidence for a low-latitude hydrologic seesaw
JF  - Scientific reports
N2  - The presence of a low-to mid-latitude interhemispheric hydrologic seesaw is apparent over orbital and glacial-interglacial timescales, but its existence over the most recent past remains unclear. Here we investigate, based on climate proxy reconstructions from both hemispheres, the inter-hemispherical phasing of the Intertropical Convergence Zone (ITCZ) and the low-to mid-latitude teleconnections in the Northern Hemisphere over the past 2000 years. A clear feature is a persistent southward shift of the ITCZ during the Little Ice Age until the beginning of the 19th Century. Strong covariation between our new composite ITCZ-stack and North Atlantic Oscillation (NAO) records reveals a tight coupling between these two synoptic weather and climate phenomena over decadal-to-centennial timescales. This relationship becomes most apparent when comparing two precisely dated, high-resolution paleorainfall records from Belize and Scotland, indicating that the low-to mid-latitude teleconnection was also active over annual-decadal timescales. It is likely a combination of external forcing, i.e., solar and volcanic, and internal feedbacks, that drives the synchronous ITCZ and NAO shifts via energy flux perturbations in the tropics.
Y1  - 2017
U6  - https://doi.org/10.1038/srep45809
SN  - 2045-2322
VL  - 7
PB  - Nature Publ. Group
CY  - London
ER  - 
TY  - JOUR
A1  - Davidsen, Joern
A1  - Kwiatek, Grzegorz
A1  - Charalampidou, Elli-Maria
A1  - Goebel, Thomas
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  - Martinez-Nunez, Silvia
A1  - Kretschmar, Peter
A1  - Bozzo, Enrico
A1  - Oskinova, Lida
A1  - Puls, Joachim
A1  - Sidoli, Lara
A1  - Sundqvist, Jon Olof
A1  - Blay, Pere
A1  - Falanga, Maurizio
A1  - Furst, Felix
A1  - Gimenez-Garcia, Angel
A1  - Kreykenbohm, Ingo
A1  - Kuehnel, Matthias
A1  - Sander, Andreas Alexander Christoph
A1  - Torrejon, Jose Miguel
A1  - Wilms, Joern
T1  - Towards a Unified View of Inhomogeneous Stellar Winds in Isolated Supergiant Stars and Supergiant High Mass X-Ray Binaries
JF  - Space science reviews
N2  - Massive stars, at least similar to 10 times more massive than the Sun, have two key properties that make them the main drivers of evolution of star clusters, galaxies, and the Universe as a whole. On the one hand, the outer layers of massive stars are so hot that they produce most of the ionizing ultraviolet radiation of galaxies; in fact, the first massive stars helped to re-ionize the Universe after its Dark Ages. Another important property of massive stars are the strong stellar winds and outflows they produce. This mass loss, and finally the explosion of a massive star as a supernova or a gamma-ray burst, provide a significant input of mechanical and radiative energy into the interstellar space. These two properties together make massive stars one of the most important cosmic engines: they trigger the star formation and enrich the interstellar medium with heavy elements, that ultimately leads to formation of Earth-like rocky planets and the development of complex life. The study of massive star winds is thus a truly multidisciplinary field and has a wide impact on different areas of astronomy. In recent years observational and theoretical evidences have been growing that these winds are not smooth and homogeneous as previously assumed, but rather populated by dense "clumps". The presence of these structures dramatically affects the mass loss rates derived from the study of stellar winds. Clump properties in isolated stars are nowadays inferred mostly through indirect methods (i.e., spectroscopic observations of line profiles in various wavelength regimes, and their analysis based on tailored, inhomogeneous wind models). The limited characterization of the clump physical properties (mass, size) obtained so far have led to large uncertainties in the mass loss rates from massive stars. Such uncertainties limit our understanding of the role of massive star winds in galactic and cosmic evolution. Supergiant high mass X-ray binaries (SgXBs) are among the brightest X-ray sources in the sky. A large number of them consist of a neutron star accreting from the wind of a massive companion and producing a powerful X-ray source. The characteristics of the stellar wind together with the complex interactions between the compact object and the donor star determine the observed X-ray output from all these systems. Consequently, the use of SgXBs for studies of massive stars is only possible when the physics of the stellar winds, the compact objects, and accretion mechanisms are combined together and confronted with observations. This detailed review summarises the current knowledge on the theory and observations of winds from massive stars, as well as on observations and accretion processes in wind-fed high mass X-ray binaries. The aim is to combine in the near future all available theoretical diagnostics and observational measurements to achieve a unified picture of massive star winds in isolated objects and in binary systems.
KW  - Massive stars
KW  - Stellar outflows
KW  - X-ray binary
KW  - Wind-fed systems
KW  - Accretion processes
KW  - SgXBs
KW  - SFXTs
Y1  - 2017
U6  - https://doi.org/10.1007/s11214-017-0340-1
SN  - 0038-6308
SN  - 1572-9672
VL  - 212
SP  - 59
EP  - 150
PB  - Springer
CY  - Dordrecht
ER  - 
TY  - JOUR
A1  - Fondell, Mattis
A1  - Eckert, Sebastian
A1  - Jay, Raphael Martin
A1  - Weniger, Christian
A1  - Quevedo, Wilson
A1  - Niskanen, Johannes
A1  - Kennedy, Brian
A1  - Sorgenfrei, Florian
A1  - Schick, Daniel
A1  - Giangrisostomi, Erika
A1  - Ovsyannikov, Ruslan
A1  - Adamczyk, Katrin
A1  - Huse, Nils
A1  - Wernet, Philippe
A1  - Mitzner, Rolf
A1  - Föhlisch, Alexander
T1  - Time-resolved soft X-ray absorption spectroscopy in transmission mode on liquids at MHz repetition rates
JF  - Structural dynamics
N2  - We present a setup combining a liquid flatjet sample delivery and a MHz laser system for time-resolved soft X-ray absorption measurements of liquid samples at the high brilliance undulator beamline UE52-SGM at Bessy II yielding unprecedented statistics in this spectral range. We demonstrate that the efficient detection of transient absorption changes in transmission mode enables the identification of photoexcited species in dilute samples. With iron(II)-trisbipyridine in aqueous solution as a benchmark system, we present absorption measurements at various edges in the soft X-ray regime. In combination with the wavelength tunability of the laser system, the set-up opens up opportunities to study the photochemistry of many systems at low concentrations, relevant to materials sciences, chemistry, and biology. (C) 2017 Author(s).
Y1  - 2017
U6  - https://doi.org/10.1063/1.4993755
SN  - 2329-7778
VL  - 4
PB  - American Institute of Physics
CY  - Melville
ER  - 
TY  - JOUR
A1  - Cherstvy, Andrey G.
A1  - Vinod, Deepak
A1  - Aghion, Erez
A1  - Chechkin, Aleksei V.
A1  - Metzler, Ralf
T1  - Time averaging, ageing and delay analysis of financial time series
JF  - New journal of physics
N2  - We introduce three strategies for the analysis of financial time series based on time averaged observables. These comprise the time averaged mean squared displacement (MSD) as well as the ageing and delay time methods for varying fractions of the financial time series. We explore these concepts via statistical analysis of historic time series for several Dow Jones Industrial indices for the period from the 1960s to 2015. Remarkably, we discover a simple universal law for the delay time averaged MSD. The observed features of the financial time series dynamics agree well with our analytical results for the time averaged measurables for geometric Brownian motion, underlying the famed Black–Scholes–Merton model. The concepts we promote here are shown to be useful for financial data analysis and enable one to unveil new universal features of stock market dynamics.
KW  - time averaging
KW  - diffusion
KW  - geometric Brownian motion
KW  - financial time series
Y1  - 2017
U6  - https://doi.org/10.1088/1367-2630/aa7199
SN  - 1367-2630
VL  - 19
SP  - 1
EP  - 11
PB  - IOP
CY  - London
ER  - 
TY  - GEN
A1  - Cherstvy, Andrey G.
A1  - Vinod, Deepak
A1  - Aghion, Erez
A1  - Chechkin, Aleksei V.
A1  - Metzler, Ralf
T1  - Time averaging, ageing and delay analysis of financial time series
N2  - We introduce three strategies for the analysis of financial time series based on time averaged observables. These comprise the time averaged mean squared displacement (MSD) as well as the ageing and delay time methods for varying fractions of the financial time series. We explore these concepts via statistical analysis of historic time series for several Dow Jones Industrial indices for the period from the 1960s to 2015. Remarkably, we discover a simple universal law for the delay time averaged MSD. The observed features of the financial time series dynamics agree well with our analytical results for the time averaged measurables for geometric Brownian motion, underlying the famed Black–Scholes–Merton model. The concepts we promote here are shown to be useful for financial data analysis and enable one to unveil new universal features of stock market dynamics.
T3  - Zweitveröffentlichungen der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe - 347 
KW  - diffusion
KW  - financial time series
KW  - geometric Brownian motion
KW  - time averaging
Y1  - 2017
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-400541
ER  - 
TY  - JOUR
A1  - Cherstvy, Andrey G.
A1  - Vinod, Deepak
A1  - Aghion, Erez
A1  - Chechkin, Aleksei V.
A1  - Metzler, Ralf
T1  - Time averaging, ageing and delay analysis of financial time series
JF  - New journal of physics : the open-access journal for physics
N2  - We introduce three strategies for the analysis of financial time series based on time averaged observables. These comprise the time averaged mean squared displacement (MSD) as well as the ageing and delay time methods for varying fractions of the financial time series. We explore these concepts via statistical analysis of historic time series for several Dow Jones Industrial indices for the period from the 1960s to 2015. Remarkably, we discover a simple universal law for the delay time averaged MSD. The observed features of the financial time series dynamics agree well with our analytical results for the time averaged measurables for geometric Brownian motion, underlying the famed Black-Scholes-Merton model. The concepts we promote here are shown to be useful for financial data analysis and enable one to unveil new universal features of stock market dynamics.
KW  - time averaging
KW  - diffusion
KW  - geometric Brownian motion
KW  - financial time series
Y1  - 2017
U6  - https://doi.org/10.1088/1367-2630/aa7199
SN  - 1367-2630
VL  - 19
SP  - 135
EP  - 147
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  - 
TY  - JOUR
A1  - Sun, Ning-Chen
A1  - de Grijs, Richard
A1  - Subramanian, Smitha
A1  - Bekki, Kenji
A1  - Bell, Cameron P. M.
A1  - Cioni, Maria-Rosa L.
A1  - Ivanov, Valentin D.
A1  - Marconi, Marcella
A1  - Oliveira, Joana M.
A1  - Piatti, Andres E.
A1  - Ripepi, Vincenzo
A1  - Rubele, Stefano
A1  - Tatton, Ben L.
A1  - van Loon, Jacco Th.
T1  - The VMC Survey. XXII. Hierarchical Star Formation in the 30 Doradus-N158–N159–N160 Star-forming Complex
JF  - The astrophysical journal : an international review of spectroscopy and astronomical physics
N2  - Star formation is a hierarchical process, forming young stellar structures of star clusters, associations, and complexes over a wide range of scales. The star-forming complex in the bar region of the Large Magellanic Cloud is investigated with upper main-sequence stars observed by the VISTA Survey of the Magellanic Clouds. The upper main-sequence stars exhibit highly nonuniform distributions. Young stellar structures inside the complex are identified from the stellar density map as density enhancements of different significance levels. We find that these structures are hierarchically organized such that larger, lower-density structures contain one or several smaller, higher-density ones. They follow power-law size and mass distributions, as well as a lognormal surface density distribution. All these results support a scenario of hierarchical star formation regulated by turbulence. The temporal evolution of young stellar structures is explored by using subsamples of upper main-sequence stars with different magnitude and age ranges. While the youngest subsample, with a median age of log(tau/yr) = 7.2, contains the most substructure, progressively older ones are less and less substructured. The oldest subsample, with a median age of log(tau/yr) = 8.0, is almost indistinguishable from a uniform distribution on spatial scales of 30-300. pc, suggesting that the young stellar structures are completely dispersed on a timescale of similar to 100. Myr. These results are consistent with the characteristics of the 30. Doradus complex and the entire Large Magellanic Cloud, suggesting no significant environmental effects. We further point out that the fractal dimension may be method dependent for stellar samples with significant age spreads.
KW  - infrared: stars
KW  - Magellanic Clouds
KW  - stars: formation
Y1  - 2017
U6  - https://doi.org/10.3847/1538-4357/aa911e
SN  - 0004-637X
SN  - 1538-4357
VL  - 849
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  - 
TY  - JOUR
A1  - Sun, Ning-Chen
A1  - de Grijs, Richard
A1  - Subramanian, Smitha
A1  - Cioni, Maria-Rosa L.
A1  - Rubele, Stefano
A1  - Bekki, Kenji
A1  - Ivanov, Valentin D.
A1  - Piatti, Andrés E.
A1  - Ripepi, Vincenzo
T1  - The VMC Survey. XXII. Hierarchical star formation in the 30 Doradus-N158-N159-N160 star-forming complex
JF  - The astrophysical journal : an international review of spectroscopy and astronomical physics
N2  - We study the hierarchical stellar structures in a similar to 1.5 deg(2) area covering the 30. Doradus-N158-N159-N160 starforming complex with the VISTA Survey of. Magellanic Clouds. Based on the young upper main-sequence stars, we find that the surface densities cover a wide range of values, from log(Sigma.pc(2))less than or similar to -2.0 to log(Sigma. pc(2)) greater than or similar to 0.0. Their distributions are highly non-uniform, showing groups that frequently have subgroups inside. The sizes of the stellar groups do not exhibit characteristic values, and range continuously from several parsecs to more than 100. pc; the cumulative size distribution can be well described by a single power law, with the power-law index indicating a projected fractal dimension D-2 = 1.6 +/- 0.3. We suggest that the phenomena revealed here support a scenario of hierarchical star formation. Comparisons with other star-forming regions and galaxies are also discussed.
KW  - galaxies: clusters: general
KW  - infrared: stars
KW  - Magellanic Clouds
KW  - stars: formation
Y1  - 2017
U6  - https://doi.org/10.3847/1538-4357/835/2/171
SN  - 0004-637X
SN  - 1538-4357
VL  - 835
IS  - 2
PB  - Institute of Physics Publ.
CY  - Bristol
ER  - 
TY  - JOUR
A1  - Subramanian, Smitha
A1  - Rubele, Stefano
A1  - Sun, Ning-Chen
A1  - Girardi, Leo
A1  - de Grijs, Richard
A1  - van Loon, Jacco Th.
A1  - Cioni, Maria-Rosa L.
A1  - Piatti, Andres E.
A1  - Bekki, Kenji
A1  - Emerson, Jim
A1  - Ivanov, Valentin D.
A1  - Kerber, Leandro
A1  - Marconi, Marcella
A1  - Ripepi, Vincenzo
A1  - Tatton, Benjamin L.
T1  - The VMC Survey - XXIV. Signatures of tidally stripped stellar populations from the inner Small Magellanic Cloud
JF  - Monthly notices of the Royal Astronomical Society
KW  - stars: individual: red clump stars
KW  - galaxies: interactions
KW  - Magellanic Clouds
Y1  - 2017
U6  - https://doi.org/10.1093/mnras/stx205
SN  - 0035-8711
SN  - 1365-2966
VL  - 467
SP  - 2980
EP  - 2995
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Richardson, Noel D.
A1  - Russell, Christopher M. P.
A1  - St-Jean, Lucas
A1  - Moffat, Anthony F. J.
A1  - St-Louis, Nicole
A1  - Shenar, Tomer
A1  - Pablo, Herbert
A1  - Hill, Grant M.
A1  - Ramiaramanantsoa, Tahina
A1  - Corcoran, Michael
A1  - Hamuguchi, Kenji
A1  - Eversberg, Thomas
A1  - Miszalski, Brent
A1  - Chene, Andre-Nicolas
A1  - Waldron, Wayne
A1  - Kotze, Enrico J.
A1  - Kotze, Marissa M.
A1  - Luckas, Paul
A1  - Cacella, Paulo
A1  - Heathcote, Bernard
A1  - Powles, Jonathan
A1  - Bohlsen, Terry
A1  - Locke, Malcolm
A1  - Handler, Gerald
A1  - Kuschnig, Rainer
A1  - Pigulski, Andrzej
A1  - Popowicz, Adam
A1  - Wade, Gregg A.
A1  - Weiss, Werner W.
T1  - The variability of the BRITE-est Wolf-Rayet binary, gamma(2) Velorum-I. Photometric and spectroscopic evidence for colliding winds
JF  - Monthly notices of the Royal Astronomical Society
N2  - We report on the first multi-colour precision light curve of the bright Wolf-Rayet binary gamma(2) Velorum, obtained over six months with the nanosatellites in the BRITE-Constellation fleet. In parallel, we obtained 488 high-resolution optical spectra of the system. In this first report on the data sets, we revise the spectroscopic orbit and report on the bulk properties of the colliding winds. We find a dependence of both the light curve and excess emission properties that scales with the inverse of the binary separation. When analysing the spectroscopic properties in combination with the photometry, we find that the phase dependence is caused only by excess emission in the lines, and not from a changing continuum. We also detect a narrow, high-velocity absorption component from the He perpendicular to lambda 5876 transition, which appears twice in the orbit. We calculate smoothed-particle hydrodynamical simulations of the colliding winds and can accurately associate the absorption from He perpendicular to to the leading and trailing arms of the wind shock cone passing tangentially through our line of sight. The simulations also explain the general strength and kinematics of the emission excess observed in wind lines such as C III lambda 5696 of the system. These results represent the first in a series of investigations into the winds and properties of gamma(2) Velorum through multi-technique and multi-wavelength observational campaigns.
KW  - stars: early type
KW  - stars: individual: gamma(2) Vel
KW  - stars: mass loss
KW  - stars: winds
KW  - outflows
KW  - stars: Wolf-Rayet
Y1  - 2017
U6  - https://doi.org/10.1093/mnras/stx1731
SN  - 0035-8711
SN  - 1365-2966
VL  - 471
SP  - 2715
EP  - 2729
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Almeida, Leonardo A.
A1  - Sana, H.
A1  - Taylor, W.
A1  - Barbá, Rodolfo
A1  - Bonanos, Alceste Z.
A1  - Crowther, Paul
A1  - Damineli, Augusto
A1  - de Koter, A.
A1  - de Mink, Selma E.
A1  - Evans, C. J.
A1  - Gieles, Mark
A1  - Grin, Nathan J.
A1  - Hénault-Brunet, V.
A1  - Langer, Norbert
A1  - Lennon, D.
A1  - Lockwood, Sean
A1  - Maíz Apellániz, Jesús
A1  - Moffat, A. F. J.
A1  - Neijssel, C.
A1  - Norman, C.
A1  - Ramírez-Agudelo, O. H.
A1  - Richardson, N. D.
A1  - Schootemeijer, Abel
A1  - Shenar, Tomer
A1  - Soszyński, Igor
A1  - Tramper, Frank
A1  - Vink, J. S.
T1  - The tarantula massive binary monitoring
BT  - I. Observational campaign and OB-type spectroscopic binaries
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context:
Massive binaries play a crucial role in the Universe. Knowing the distributions of their orbital parameters is important for a wide range of topics from stellar feedback to binary evolution channels and from the distribution of supernova types to gravitational wave progenitors, yet no direct measurements exist outside the Milky Way.
Aims:
The Tarantula Massive Binary Monitoring project was designed to help fill this gap by obtaining multi-epoch radial velocity (RV) monitoring of 102 massive binaries in the 30 Doradus region.
Methods: 
In this paper we analyze 32 FLAMES/GIRAFFE observations of 93 O- and 7 B-type binaries. We performed a Fourier analysis and obtained orbital solutions for 82 systems: 51 single-lined (SB1) and 31 double-lined (SB2) spectroscopic binaries.
Results: 
Overall, the binary fraction and orbital properties across the 30 Doradus region are found to be similar to existing Galactic samples. This indicates that within these domains environmental effects are of second order in shaping the properties of massive binary systems. A small difference is found in the distribution of orbital periods, which is slightly flatter (in log space) in 30 Doradus than in the Galaxy, although this may be compatible within error estimates and differences in the fitting methodology. Also, orbital periods in 30 Doradus can be as short as 1.1 d, somewhat shorter than seen in Galactic samples. Equal mass binaries (q> 0.95) in 30 Doradus are all found outside NGC 2070, the central association that surrounds R136a, the very young and massive cluster at 30 Doradus’s core. Most of the differences, albeit small, are compatible with expectations from binary evolution. One outstanding exception, however, is the fact that earlier spectral types (O2–O7) tend to have shorter orbital periods than later spectral types (O9.2–O9.7).
Conclusions: 
Our results point to a relative universality of the incidence rate of massive binaries and their orbital properties in the metallicity range from solar (Z⊙) to about half solar. This provides the first direct constraints on massive binary properties in massive star-forming galaxies at the Universe’s peak of star formation at redshifts z ~ 1 to 2 which are estimated to have Z ~ 0.5 Z⊙.
KW  - stars: early-type
KW  - stars: massive
KW  - binaries: spectroscopic
KW  - binaries: close
Y1  - 2017
U6  - https://doi.org/10.1051/0004-6361/201629844
SN  - 1432-0746
VL  - 598
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Shenar, Tomer
A1  - Richardson, N. D.
A1  - Sablowski, Daniel P.
A1  - Hainich, Rainer
A1  - Sana, H.
A1  - Moffat, A. F. J.
A1  - Todt, Helge Tobias
A1  - Hamann, Wolf-Rainer
A1  - Oskinova, Lida
A1  - Sander, Andreas Alexander Christoph
A1  - Tramper, Frank
A1  - Langer, Norbert
A1  - Bonanos, Alceste Z.
A1  - de Mink, Selma E.
A1  - Gräfener, G.
A1  - Crowther, Paul
A1  - Vink, J. S.
A1  - Almeida, Leonardo A.
A1  - de Koter, A.
A1  - Barbá, Rodolfo
A1  - Herrero, A.
A1  - Ulaczyk, Krzysztof
T1  - The tarantula massive binary monitoring
BT  - II. First SB2 orbital and spectroscopic analysis for the Wolf-Rayet binary R145
JF  - Astronomy and astrophysics : an international weekly journal
N2  - We present the first SB2 orbital solution and disentanglement of the massive Wolf-Rayet binary R145 (P = 159 d) located in the Large Magellanic Cloud. The primary was claimed to have a stellar mass greater than 300 M-circle dot, making it a candidate for being the most massive star known to date. While the primary is a known late-type, H-rich Wolf-Rayet star (WN6h), the secondary has so far not been unambiguously detected. Using moderate-resolution spectra, we are able to derive accurate radial velocities for both components. By performing simultaneous orbital and polarimetric analyses, we derive the complete set of orbital parameters, including the inclination. The spectra are disentangled and spectroscopically analyzed, and an analysis of the wind-wind collision zone is conducted. The disentangled spectra and our models are consistent with a WN6h type for the primary and suggest that the secondary is an O3.5 If*/WN7 type star. We derive a high eccentricity of e = 0 : 78 and minimum masses of M-1 sin(3) i approximate to M-2 sin(3) i = 13 +/- 2 M-circle dot, with q = M-2/M-1 = 1.01 +/- 0.07. An analysis of emission excess stemming from a wind-wind collision yields an inclination similar to that obtained from polarimetry (i = 39 +/- 6 degrees). Our analysis thus implies M-1 = 53(-20)(+40) and M2 = 54(-20)(+40) M-circle dot, excluding M-1 > 300 M-circle dot. A detailed comparison with evolution tracks calculated for single and binary stars together with the high eccentricity suggests that the components of the system underwent quasi-homogeneous evolution and avoided mass-transfer. This scenario would suggest current masses of approximate to 80 M-circle dot and initial masses of M-i,M-1 approximate to 10(5) and M-i,M-2 approximate to 90 M-circle dot, consistent with the upper limits of our derived orbital masses, and would imply an age of approximate to 2.2 Myr.
KW  - binaries: spectroscopic
KW  - stars: Wolf-Rayet
KW  - stars: massive
KW  - Magellanic Clouds
KW  - stars: individual: R 145
KW  - stars: atmospheres
Y1  - 2017
U6  - https://doi.org/10.1051/0004-6361/201629621
SN  - 1432-0746
VL  - 598
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Bozzo, Enrico
A1  - Oskinova, Lida
A1  - Lobel, A.
A1  - Hamann, Wolf-Rainer
T1  - The super-orbital modulation of supergiant high-mass X-ray binaries
JF  - Astronomy and astrophysics : an international weekly journal
N2  - The long-term X-ray light curves of classical supergiant X-ray binaries and supergiant fast X-ray transients show relatively similar super-orbital modulations, which are still lacking a sound interpretation. We propose that these modulations are related to the presence of corotating interaction regions (CIRs) known to thread the winds of OB supergiants. To test this hypothesis, we couple the outcomes of three-dimensional (3D) hydrodynamic models for the formation of CIRs in stellar winds with a simplified recipe for the accretion onto a neutron star. The results show that the synthetic X-ray light curves are indeed modulated by the presence of the CIRs. The exact period and amplitude of these modulations depend on a number of parameters governing the hydrodynamic wind models and on the binary orbital configuration. To compare our model predictions with the observations, we apply the 3D wind structure previously shown to well explain the appearance of discrete absorption components in the UV time series of a prototypical B0.5I-type supergiant. Using the orbital parameters of IGRJ 16493-4348, which has the same B0.5I donor spectral type, the period and modulations in the simulated X-ray light curve are similar to the observed ones, thus providing support to our scenario. We propose that the presence of CIRs in donor star winds should be considered in future theoretical and simulation efforts of wind-fed X-ray binaries.
KW  - X-rays: stars
KW  - X-rays: binaries
KW  - gamma rays: stars
KW  - stars: massive
KW  - stars: neutron
Y1  - 2017
U6  - https://doi.org/10.1051/0004-6361/201731930
SN  - 1432-0746
VL  - 606
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Xiong, Hui
A1  - Mignolet, Benoit
A1  - Fang, Li
A1  - Osipov, Timur
A1  - Wolf, Thomas J. A.
A1  - Sistrunk, Emily
A1  - Gühr, Markus
A1  - Remacle, Francoise
A1  - Berrah, Nora
T1  - The Role of Super-Atom Molecular Orbitals in Doped Fullerenes in a Femtosecond Intense Laser Field
JF  - Scientific reports
N2  - The interaction of gas phase endohedral fullerene Ho3N@C-80 with intense (0.1-5 x 10(14) W/cm(2)), short (30 fs), 800 nm laser pulses was investigated. The power law dependence of Ho3N@C-80(q+), q = 1-2, was found to be different from that of C-60. Time-dependent density functional theory computations revealed different light-induced ionization mechanisms. Unlike in C-60, in doped fullerenes, the breaking of the cage spherical symmetry makes super atomic molecular orbital (SAMO) states optically active. Theoretical calculations suggest that the fast ionization of the SAMO states in Ho3N@C-80 is responsible for the n = 3 power law for singly charged parent molecules at intensities lower than 1.2 x 10(14) W/cm(2).
Y1  - 2017
U6  - https://doi.org/10.1038/s41598-017-00124-9
SN  - 2045-2322
VL  - 7
PB  - Nature Publ. Group
CY  - London
ER  - 
TY  - JOUR
A1  - Starkenburg, Else
A1  - Martin, Nicolas
A1  - Youakim, Kris
A1  - Aguado, David S.
A1  - Allende Prieto, Carlos
A1  - Arentsen, Anke
A1  - Bernard, Edouard J.
A1  - Bonifacio, Piercarlo
A1  - Caffau, Elisabetta
A1  - Carlberg, Raymond G.
A1  - Cote, Patrick
A1  - Fouesneau, Morgan
A1  - Francois, Patrick
A1  - Franke, Oliver
A1  - Gonzalez Hernandez, Jonay I.
A1  - Gwyn, Stephen D. J.
A1  - Hill, Vanessa
A1  - Ibata, Rodrigo A.
A1  - Jablonka, Pascale
A1  - Longeard, Nicolas
A1  - McConnachie, Alan W.
A1  - Navarro, Julio F.
A1  - Sanchez-Janssen, Ruben
A1  - Tolstoy, Eline
A1  - Venn, Kim A.
T1  - The Pristine survey - I. Mining the Galaxy for the most metal-poor stars
JF  - Monthly notices of the Royal Astronomical Society
N2  - We present the Pristine survey, a new narrow-band photometric survey focused on the metallicity-sensitive Ca H&K lines and conducted in the Northern hemisphere with the wide-field imager MegaCam on the Canada-France-Hawaii Telescope. This paper reviews our overall survey strategy and discusses the data processing and metallicity calibration. Additionally we review the application of these data to the main aims of the survey, which are to gather a large sample of the most metal-poor stars in the Galaxy, to further characterize the faintest Milky Way satellites, and to map the (metal-poor) substructure in the Galactic halo. The current Pristine footprint comprises over 1000 deg(2) in the Galactic halo ranging from b similar to 30 degrees to similar to 78 degrees and covers many known stellar substructures. We demonstrate that, for Sloan Digital Sky Survey (SDSS) stellar objects, we can calibrate the photometry at the 0.02-mag level. The comparison with existing spectroscopic metallicities from SDSS/Sloan Extension for Galactic Understanding and Exploration (SEGUE) and Large Sky Area Multi-Object Fiber Spectroscopic Telescope shows that, when combined with SDSS broad-band g and i photometry, we can use the CaHK photometry to infer photometric metallicities with an accuracy of similar to 0.2 dex from [Fe/H] = -0.5 down to the extremely metal-poor regime ([Fe/H] < -3.0). After the removal of various contaminants, we can efficiently select metal-poor stars and build a very complete sample with high purity. The success rate of uncovering [Fe/H](SEGUE) < -3.0 stars among [Fe/H](Pristine) < -3.0 selected stars is 24 per cent, and 85 per cent of the remaining candidates are still very metal poor ([Fe/H]<-2.0). We further demonstrate that Pristine is well suited to identify the very rare and pristine Galactic stars with [Fe/H] < -4.0, which can teach us valuable lessons about the early Universe.
KW  - stars: abundances
KW  - Galaxy: abundances
KW  - Galaxy: evolution
KW  - Galaxy: formation
KW  - Galaxy: halo
KW  - galaxies: dwarf
Y1  - 2017
U6  - https://doi.org/10.1093/mnras/stx1068
SN  - 0035-8711
SN  - 1365-2966
VL  - 471
SP  - 2587
EP  - 2604
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - THES
A1  - Feulner, Georg
T1  - The influence of solar radiation changes on the energy budget of Earth's climate
Y1  - 2017
ER  - 
TY  - GEN
A1  - Parsons, R. D.
A1  - Schüssler, F.
A1  - Garrigoux, T.
A1  - Balzer, A.
A1  - Füssling, Matthias
A1  - Hoischen, Clemens
A1  - Holler, M.
A1  - Mitchell, A.
A1  - Pühlhofer, G.
A1  - Rowell, G.
A1  - Wagner, S.
A1  - Bissaldi, E.
A1  - Tam, P. H. T.
T1  - The HESS II GRB Observation Scheme
T2  - AIP conference proceedings / American Institute of Physics
N2  - Gamma-ray bursts (GRBs) are some of the Universe’s most enigmatic and exotic events. However, at energies above 10 GeV their behaviour remains largely unknown. Although space based telescopes such as the Fermi-LAT have been able to detect GRBs in this energy range, their photon statistics are limited by the small detector size. Such limitations are not present in ground based gamma-ray telescopes such as the H.E.S.S. experiment, which has now entered its second phase with the addition of a large 600 m2 telescope to the centre of the array. Such a large telescope allows H.E.S.S. to access the sub 100-GeV energy range while still maintaining a large effective collection area, helping to potentially probe the short timescale emission of these events.
We present a description of the H.E.S.S. GRB observation programme, summarising the performance of the rapid GRB repointing system and the conditions under which GRB observations are initiated. Additionally we will report on the GRB follow-ups made during the 2014-15 observation campaigns.
Y1  - 2017
SN  - 978-0-7354-1456-3
U6  - https://doi.org/10.1063/1.4968980
SN  - 0094-243X
SN  - 1551-7616
VL  - 1792
IS  - 1
PB  - American Institute of Physics
CY  - Melville
ER  - 
TY  - JOUR
A1  - Reese, Ronja
A1  - Gudmundsson, Gudmundur Hilmar
A1  - Levermann, Anders
A1  - Winkelmann, Ricarda
T1  - The far reach of ice-shelf thinning in Antarctica
JF  - Nature climate change
N2  - Floating ice shelves, which fringe most of Antarctica’s coastline, regulate ice flow into the Southern Ocean1,2,3. Their thinning4,5,6,7 or disintegration8,9 can cause upstream acceleration of grounded ice and raise global sea levels. So far the effect has not been quantified in a comprehensive and spatially explicit manner. Here, using a finite-element model, we diagnose the immediate, continent-wide flux response to different spatial patterns of ice-shelf mass loss. We show that highly localized ice-shelf thinning can reach across the entire shelf and accelerate ice flow in regions far from the initial perturbation. As an example, this ‘tele-buttressing’ enhances outflow from Bindschadler Ice Stream in response to thinning near Ross Island more than 900 km away. We further find that the integrated flux response across all grounding lines is highly dependent on the location of imposed changes: the strongest response is caused not only near ice streams and ice rises, but also by thinning, for instance, well-within the Filchner–Ronne and Ross Ice Shelves. The most critical regions in all major ice shelves are often located in regions easily accessible to the intrusion of warm ocean waters10,11,12, stressing Antarctica’s vulnerability to changes in its surrounding ocean.
Y1  - 2017
U6  - https://doi.org/10.1038/s41558-017-0020-x
SN  - 1758-678X
SN  - 1758-6798
VL  - 8
IS  - 1
SP  - 53
EP  - 57
PB  - Nature Publ. Group
CY  - London
ER  - 
TY  - JOUR
A1  - Dzhanoev, Arsen R.
A1  - Sokolov, Igor M.
T1  - The effect of the junction model on the anomalous diffusion in the 3D comb structure
JF  - Chaos, solitons & fractals : applications in science and engineering ; an interdisciplinary journal of nonlinear science
N2  - The diffusion in the comb structures is a popular model of geometrically induced anomalous diffusion. In the present work we concentrate on the diffusion along the backbone in a system where sidebranches are planes, and the diffusion thereon is anomalous and described by continuous time random walks (CTRW). We show that the mean squared displacement (MSD) in the backbone of the comb behaves differently depending on whether the waiting time periods in the sidebranches are reset after the step in the backbone is done (a rejuvenating junction model), or not (a non-rejuvenating junction model). In the rejuvenating case the subdiffusion in the sidebranches only changes the prefactor in the ultra-slow (logarithmic) diffusion along the backbone, while in the non-rejuvenating case the ultraslow, logarithmic subdiffusion is changed to a much faster power-law subdiffusion (with a logarithmic correction) as it was found earlier by Iomin and Mendez [25]. Moreover, in the first case the result does not change if the diffusion in the backbone is itself anomalous, while in the second case it does. Two of the special cases of the considered models (the non-rejuvenating junction under normal diffusion in the backbone, and rejuvenating junction for the same waiting time distribution in the sidebranches and in junction points) were also investigated within the approach based on the corresponding generalized Fokker-Planck equations. (c) 2017 Elsevier Ltd. All rights reserved.
KW  - Comb model
KW  - Comb-lattice model
KW  - Cylindrical comb
KW  - Junction model
KW  - Anomalous diffusion
Y1  - 2017
U6  - https://doi.org/10.1016/j.chaos.2017.12.001
SN  - 0960-0779
SN  - 1873-2887
VL  - 106
SP  - 330
EP  - 336
PB  - Elsevier
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Pillitteri, Ignazio
A1  - Wolk, Scott J.
A1  - Reale, Fabio
A1  - Oskinova, Lida
T1  - The early B-type star Rho Ophiuchi A is an X-ray lighthouse
JF  - Astronomy and astrophysics : an international weekly journal
N2  - We present the results of a 140 ks XMM-Newton observation of the B2 star rho Oph A. The star has exhibited strong X-ray variability: a cusp-shaped increase of rate, similar to that which we partially observed in 2013, and a bright flare. These events are separated in time by about 104 ks, which likely correspond to the rotational period of the star (1.2 days). Time resolved spectroscopy of the X-ray spectra shows that the first event is caused by an increase of the plasma emission measure, while the second increase of rate is a major flare with temperatures in excess of 60 MK (kT similar to 5 keV). From the analysis of its rise, we infer a magnetic field of >= 300 G and a size of the flaring region of similar to 1.4-1.9 x 10(11) cm, which corresponds to similar to 25%-30% of the stellar radius. We speculate that either an intrinsic magnetism that produces a hot spot on its surface or an unknown low mass companion are the source of such X-rays and variability. A hot spot of magnetic origin should be a stable structure over a time span of >= 2.5 yr, and suggests an overall large scale dipolar magnetic field that produces an extended feature on the stellar surface. In the second scenario, a low mass unknown companion is the emitter of X-rays and it should orbit extremely close to the surface of the primary in a locked spin-orbit configuration, almost on the verge of collapsing onto the primary. As such, the X-ray activity of the secondary star would be enhanced by its young age, and the tight orbit as in RS Cvn systems. In both cases rho Oph would constitute an extreme system that is worthy of further investigation.
KW  - stars: activity
KW  - stars: individual: Rho Ophiuchi
KW  - stars: early-type
KW  - stars: magnetic field
KW  - starspots
KW  - X-rays: stars
Y1  - 2017
U6  - https://doi.org/10.1051/0004-6361/201630070
SN  - 1432-0746
VL  - 602
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - De Angelis, A.
A1  - Tatischeff, V.
A1  - Tavani, M.
A1  - Oberlack, U.
A1  - Grenier, I.
A1  - Hanloni, L.
A1  - Walter, R.
A1  - Argan, A.
A1  - Von Ballmoos, P.
A1  - Bulgarelli, A.
A1  - Donnarumma, I.
A1  - Hernanz, M.
A1  - Kuvvetli, I.
A1  - Pearce, M.
A1  - Zdziarski, A.
A1  - Aboudan, A.
A1  - Ajello, M.
A1  - Ambrosi, G.
A1  - Bernard, D.
A1  - Bernardini, E.
A1  - Bonvicini, V.
A1  - Brogna, A.
A1  - Branchesi, M.
A1  - Budtz-Jorgensen, C.
A1  - Bykov, A. M.
A1  - Campana, R.
A1  - Cardillo, M.
A1  - Coppi, P.
A1  - De Martino, D.
A1  - Diehl, R.
A1  - Doro, M.
A1  - Fioretti, V.
A1  - Funk, S.
A1  - Ghisellini, G.
A1  - Grove, E.
A1  - Hamadache, C.
A1  - Hartmann, D. H.
A1  - Hayashida, M.
A1  - Isern, J.
A1  - Kanbach, G.
A1  - Kiener, J.
A1  - Knodlseder, J.
A1  - Labanti, C.
A1  - Laurent, P.
A1  - Limousin, O.
A1  - Longo, F.
A1  - Mannheim, K.
A1  - Marisaldi, M.
A1  - Martinez, M.
A1  - Mazziotta, Mario Nicola
A1  - McEnery, J.
A1  - Mereghetti, S.
A1  - Minervini, G.
A1  - Moiseev, A.
A1  - Morselli, A.
A1  - Nakazawa, K.
A1  - Orleanski, P.
A1  - Paredes, J. M.
A1  - Patricelli, B.
A1  - Pevre, J.
A1  - Piano, G.
A1  - Pohl, Martin
A1  - Ramarijaona, H.
A1  - Rando, R.
A1  - Reichardt, I.
A1  - Roncadelli, M.
A1  - Silva, R.
A1  - Tavecchio, F.
A1  - Thompson, D. J.
A1  - Turolla, R.
A1  - Ulyanov, A.
A1  - Vacchi, A.
A1  - Wu, X.
A1  - Zoglauer, A.
T1  - The e-ASTROGAM mission Exploring the extreme Universe with gamma rays in the MeV - GeV range
JF  - Experimental astronomy : an international journal on astronomical instrumentation and data analysis
N2  - e-ASTROGAM (‘enhanced ASTROGAM’) is a breakthrough Observatory space mission, with a detector composed by a Silicon tracker, a calorimeter, and an anticoincidence system, dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV – the lower energy limit can be pushed to energies as low as 150 keV, albeit with rapidly degrading angular resolution, for the tracker, and to 30 keV for calorimetric detection. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and the promise of eLISA.
KW  - High-Energy Gamma-Ray Astronomy
KW  - High-Energy Astrophysics
KW  - Nuclear Astrophysics
KW  - Compton and Pair Creation Telescope
KW  - Gamma-Ray Bursts
KW  - Active Galactic Nuclei
KW  - Jets
KW  - Outflows
KW  - Multiwavelength Observations of the Universe
KW  - Counterparts of gravitational waves
KW  - Fermi
KW  - Dark Matter
KW  - Nucleosynthesis
KW  - Early Universe
KW  - Supernovae
KW  - Cosmic Rays
KW  - Cosmic Antimatter
Y1  - 2017
U6  - https://doi.org/10.1007/s10686-017-9533-6
SN  - 0922-6435
SN  - 1572-9508
VL  - 44
SP  - 25
EP  - 82
PB  - Springer
CY  - Dordrecht
ER  - 
TY  - JOUR
A1  - Leto, Paolo
A1  - Trigilio, C.
A1  - Oskinova, Lida
A1  - Ignace, R.
A1  - Buemi, C. S.
A1  - Umana, G.
A1  - Ingallinera, A.
A1  - Todt, Helge Tobias
A1  - Leone, F.
T1  - The detection of variable radio emission from the fast rotating magnetic hot B-star HR 7355 and evidence for its X-ray aurorae
JF  - Monthly notices of the Royal Astronomical Society
N2  - In this paper, we investigate the multiwavelength properties of the magnetic early B-type star HR 7355. We present its radio light curves at several frequencies, taken with the Jansky Very Large Array, and X-ray spectra, taken with the XMM-Newton X-ray telescope. Modelling of the radio light curves for the Stokes I and V provides a quantitative analysis of the HR 7355 magnetosphere. A comparison between HR 7355 and a similar analysis for the Ap star CU Vir allows us to study how the different physical parameters of the two stars affect the structure of the respective magnetospheres where the non-thermal electrons originate. Our model includes a cold thermal plasma component that accumulates at high magnetic latitudes that influences the radio regime, but does not give rise to X-ray emission. Instead, the thermal X-ray emission arises from shocks generated by wind stream collisions close to the magnetic equatorial plane. The analysis of the X-ray spectrum of HR 7355 also suggests the presence of a non-thermal radiation. Comparison between the spectral index of the power-law X-ray energy distribution with the non-thermal electron energy distribution indicates that the non-thermal X-ray component could be the auroral signature of the non-thermal electrons that impact the stellar surface, the same non-thermal electrons that are responsible for the observed radio emission. On the basis of our analysis, we suggest a novel model that simultaneously explains the X-ray and the radio features of HR 7355 and is likely relevant for magnetospheres of other magnetic early-type stars.
KW  - stars: chemically peculiar
KW  - stars: early-type
KW  - stars: individual: HR 7355
KW  - stars: magnetic field
KW  - radio continuum: stars
KW  - X-rays: stars
Y1  - 2017
U6  - https://doi.org/10.1093/mnras/stx267
SN  - 0035-8711
SN  - 1365-2966
VL  - 467
SP  - 2820
EP  - 2833
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Grinberg, Victoria
A1  - Hell, Natalie
A1  - El Mellah, Ileyk
A1  - Neilsen, Joseph
A1  - Sander, Andreas Alexander Christoph
A1  - Leutenegger, Maurice
A1  - Fürst, Felix
A1  - Huenemoerder, David P.
A1  - Kretschmar, Peter
A1  - Kuehnel, Matthias
A1  - Martinez-Nunez, Silvia
A1  - Niu, Shu
A1  - Pottschmidt, Katja
A1  - Schulz, Norbert S.
A1  - Wilms, Joern
A1  - Nowak, Michael A.
T1  - The clumpy absorber in the high-mass X-ray binary Vela X-1
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Bright and eclipsing, the high-mass X-ray binary Vela X-1 offers a unique opportunity to study accretion onto a neutron star from clumpy winds of O/B stars and to disentangle the complex accretion geometry of these systems. In Chandra-HETGS spectroscopy at orbital phase similar to 0.25, when our line of sight towards the source does not pass through the large-scale accretion structure such as the accretion wake, we observe changes in overall spectral shape on timescales of a few kiloseconds. This spectral variability is, at least in part, caused by changes in overall absorption and we show that such strongly variable absorption cannot be caused by unperturbed clumpy winds of O/B stars. We detect line features from high and low ionization species of silicon, magnesium, and neon whose strengths and presence depend on the overall level of absorption. These features imply a co-existence of cool and hot gas phases in the system, which we interpret as a highly variable, structured accretion flow close to the compact object such as has been recently seen in simulations of wind accretion in high-mass X-ray binaries.
KW  - X-rays: individuals: Vela X-1
KW  - X-rays: binaries
KW  - stars: winds, outflows
KW  - stars: massive
Y1  - 2017
U6  - https://doi.org/10.1051/0004-6361/201731843
SN  - 1432-0746
VL  - 608
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Bozzo, Enrico
A1  - Bernardini, F.
A1  - Ferrigno, Carlo
A1  - Falanga, M.
A1  - Romano, Patrizia
A1  - Oskinova, Lida
T1  - The accretion environment of supergiant fast X-ray transients probed with XMM-Newton
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. Supergiant fast X-ray (SFXT) transients are a peculiar class of supergiant X-ray binaries characterized by a remarkable variability in the X-ray domain, widely ascribed to accretion from a clumpy stellar wind. Aims. In this paper we performed a systematic and homogeneous analysis of the sufficiently bright X-ray flares observed with XMM-Newton from the supergiant fast X-ray transients to probe spectral variations on timescales as short as a few hundred seconds. Our ultimate goal is to investigate whether SFXT flares and outbursts are triggered by the presence of clumps, and to reveal whether strongly or mildly dense clumps are required. Methods. For all sources, we employ a technique developed by our group already exploited in a number of our previous papers, making use of an adaptive rebinned hardness ratio to optimally select the time intervals for the spectral extraction. A total of twelve observations performed in the direction of five SFXTs are reported, providing the largest sample of events available so far. Results. Using the original results reported here and those obtained with our technique from the analysis of two previously published XMM-Newton observations of IGR J17544-2619 and IGR J18410-0535, we show that both strongly and mildly dense clumps can trigger these events. In the former case, the local absorption column density may increase by a factor of >> 3, while in the latter case, the increase is only a factor of similar to 2-3 (or lower). An increase in the absorption column density is generally recorded during the rise of the flares/outbursts, while a drop follows when the source achieves peak flux. In a few cases, a re-increase of the absorption column density after the flare is also detected, and we discovered one absorption event related to the passage of an unaccreted clump in front of the compact object. Overall, there seems to be no obvious correlation between the dynamic ranges in the X-ray fluxes and absorption column densities in supergiant fast X-ray transients, with an indication that lower densities are recorded at the highest fluxes. Conclusions. The spectral variations measured in all sources are in agreement with the idea that the flares/outbursts are triggered by the presence of dense structures in the wind interacting with the X-rays from the compact object (leading to photoionization). The lack of correlation between the dynamic ranges in the X-ray fluxes and absorption column densities can be explained by the presence of accretion inhibition mechanism(s). Based on the knowledge acquired so far on the SFXTs, we propose a classification of the flares/outbursts from these sources in order to drive future observational investigations. We suggest that the difference between the classes of flares/outbursts is related to the fact that the mechanism(s) inhibiting accretion can be overcome more easily in some sources compared to others. We also investigate the possibility that different stellar wind structures, other than clumps, could provide the means to temporarily overcome the inhibition of accretion in supergiant fast X-ray transients.
KW  - X-rays: individuals: IGRJ18450-0435
KW  - X-rays: individuals: IGRJ17544-2619
KW  - X-rays: binaries
KW  - X-rays: individuals: SAXJ1818.6-1703
KW  - X-rays: individuals: IGRJ17354-3255
KW  - X-rays: individuals: IGRJ16328-4726
Y1  - 2017
U6  - https://doi.org/10.1051/0004-6361/201730398
SN  - 1432-0746
VL  - 608
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Abdalla, Hassan E.
A1  - Abramowski, Attila
A1  - Aharonian, Felix A.
A1  - Benkhali, Faical  Ait
A1  - Anguner, Ekrem Oǧuzhan
A1  - Arakawa, M.
A1  - Arrieta, M.
A1  - Aubert, Pierre
A1  - Backes, Michael
A1  - Balzer, Arnim
A1  - Barnard, Michelle
A1  - Becherini, Yvonne
A1  - Tjus, J. Becker
A1  - Berge, David
A1  - Bernhard, Sabrina
A1  - Bernlöhr, K.
A1  - Blackwell, R.
A1  - Böttcher, Markus
A1  - Boisson, Catherine
A1  - Bolmont, J.
A1  - Bonnefoy, S.
A1  - Bordas, Pol
A1  - Bregeon, Johan
A1  - Brun, Francois
A1  - Brun, Pierre
A1  - Bryan, Mark
A1  - Buechele, M.
A1  - Bulik, Tomasz
A1  - Capasso, M.
A1  - Caroff, S.
A1  - Carosi, A.
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chakraborty, N.
A1  - Chaves, Ryan C. G.
A1  - Chen, Andrew
A1  - Chevalier, J.
A1  - Colafrancesco, Sergio
A1  - Condon, B.
A1  - Conrad, Jan
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  - Dutson, K.
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  - Giebels, B.
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, James Anthony
A1  - Hofmann, W.
A1  - Hoischen, Clemens
A1  - Holch, Tim Lukas
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  - Kruer, P. P.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lau, J.
A1  - Lees, J. -P.
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  - Poon, H.
A1  - Prokhorov, D.
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, David M.
A1  - Santangelo, A.
A1  - Sasaki, M.
A1  - Schlickeiser, R.
A1  - Schussler, 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  - 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, Iurii
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  - TeV Gamma-Ray Observations of the Binary Neutron Star Merger GW170817 with HESS
JF  - The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters
N2  - We search for high-energy gamma-ray emission from the binary neutron star merger GW170817 with the H.E.S.S. Imaging Air Cherenkov Telescopes. The observations presented here have been obtained starting only 5.3 hr after GW170817. The H.E.S.S. target selection identified regions of high probability to find a counterpart of the gravitational-wave event. The first of these regions contained the counterpart SSS17a that has been identified in the optical range several hours after our observations. We can therefore present the first data obtained by a ground-based pointing instrument on this object. A subsequent monitoring campaign with the H.E.S.S. telescopes extended over several days, covering timescales from 0.22 to 5.2 days and energy ranges between 270 GeV to 8.55 TeV. No significant gamma-ray emission has been found. The derived upper limits on the very-high-energy gamma-ray flux for the first time constrain non-thermal, high-energy emission following the merger of a confirmed binary neutron star system.
KW  - gamma-ray burst: individual (GRB 170817A)
KW  - gamma rays: general
KW  - gravitational waves
Y1  - 2017
U6  - https://doi.org/10.3847/2041-8213/aa97d2
SN  - 2041-8205
SN  - 2041-8213
VL  - 850
SP  - 628
EP  - 650
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  - 
TY  - JOUR
A1  - Lopez-Barquero, Vanessa
A1  - Xu, S.
A1  - Desiati, Paolo
A1  - Lazarian, Alex
A1  - Pogorelov, Nikolai V.
A1  - Yan, Huirong
T1  - TeV Cosmic-Ray Anisotropy from the Magnetic Field at the Heliospheric Boundary
JF  - The astrophysical journal : an international review of spectroscopy and astronomical physics
KW  - cosmic rays
KW  - magnetic fields
KW  - magnetohydrodynamics (MHD)
KW  - solar wind
KW  - Sun: heliosphere
Y1  - 2017
U6  - https://doi.org/10.3847/1538-4357/aa74d1
SN  - 0004-637X
SN  - 1538-4357
VL  - 842
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  - 
TY  - JOUR
A1  - Graves, Timothy
A1  - Franzke, Christian L. E.
A1  - Watkins, Nicholas W.
A1  - Gramacy, Robert B.
A1  - Tindale, Elizabeth
T1  - Systematic inference of the long-range dependence and heavy-tail distribution parameters of ARFIMA models
JF  - Physica : europhysics journal ; A, Statistical mechanics and its applications
KW  - Long-range dependence
KW  - Heavy-tails
KW  - Bayesian estimation
KW  - ARFIMA
Y1  - 2017
U6  - https://doi.org/10.1016/j.physa.2017.01.028
SN  - 0378-4371
SN  - 1873-2119
VL  - 473
SP  - 60
EP  - 71
PB  - Elsevier
CY  - Amsterdam
ER  - 
TY  - JOUR
A1  - Dolmatova, Anastasiya V.
A1  - Goldobin, Denis S.
A1  - Pikovskij, Arkadij
T1  - Synchronization of coupled active rotators by common noise
JF  - Physical review : E, Statistical, nonlinear and soft matter physics
N2  - We study the effect of common noise on coupled active rotators. While such a noise always facilitates synchrony, coupling may be attractive (synchronizing) or repulsive (desynchronizing). We develop an analytical approach based on a transformation to approximate angle-action variables and averaging over fast rotations. For identical rotators, we describe a transition from full to partial synchrony at a critical value of repulsive coupling. For nonidentical rotators, the most nontrivial effect occurs at moderate repulsive coupling, where a juxtaposition of phase locking with frequency repulsion (anti-entrainment) is observed. We show that the frequency repulsion obeys a nontrivial power law.
Y1  - 2017
U6  - https://doi.org/10.1103/PhysRevE.96.062204
SN  - 2470-0045
SN  - 2470-0053
VL  - 96
SP  - E10648
EP  - E10657
PB  - American Physical Society
CY  - College Park
ER  - 
TY  - JOUR
A1  - Gout, Julien
A1  - Quade, Markus
A1  - Shafi, Kamran
A1  - Niven, Robert K.
A1  - Abel, Markus
T1  - Synchronization control of oscillator networks using symbolic regression
JF  - Nonlinear Dynamics
N2  - Networks of coupled dynamical systems provide a powerful way to model systems with enormously complex dynamics, such as the human brain. Control of synchronization in such networked systems has far-reaching applications in many domains, including engineering and medicine. In this paper, we formulate the synchronization control in dynamical systems as an optimization problem and present a multi-objective genetic programming-based approach to infer optimal control functions that drive the system from a synchronized to a non-synchronized state and vice versa. The genetic programming-based controller allows learning optimal control functions in an interpretable symbolic form. The effectiveness of the proposed approach is demonstrated in controlling synchronization in coupled oscillator systems linked in networks of increasing order complexity, ranging from a simple coupled oscillator system to a hierarchical network of coupled oscillators. The results show that the proposed method can learn highly effective and interpretable control functions for such systems.
KW  - Dynamical systems
KW  - Synchronization control
KW  - Genetic programming
Y1  - 2017
U6  - https://doi.org/10.1007/s11071-017-3925-z
SN  - 0924-090X
SN  - 1573-269X
VL  - 91
IS  - 2
SP  - 1001
EP  - 1021
PB  - Springer
CY  - Dordrecht
ER  - 
TY  - GEN
A1  - Loupos, Konstantinos
A1  - Damigos, Yannis
A1  - Amditis, Angelos
A1  - Gerhard, Reimund
A1  - Rychkov, Dmitry
A1  - Wirges, Werner
A1  - Schulze, Manuel
A1  - Lenas, Sotiris-Angelos
A1  - Chatziandreoglou, Christos
A1  - Malliou, Christina
A1  - Tsaoussidis, Vassilis
A1  - Brady, Ken
A1  - Frankenstein, Bernd
T1  - Structural health monitoring system for bridges based on skin-like sensor
T2  - IOP conference series : Materials science and engineering
N2  - Structural health monitoring activities are of primal importance for managing transport infrastructure, however most SHM methodologies are based on point-based sensors that have limitations in terms of their spatial positioning requirements, cost of development and measurement range. This paper describes the progress on the SENSKIN EC project whose objective is to develop a dielectric-elastomer and micro-electronics-based sensor, formed from a large highly extensible capacitance sensing membrane supported by advanced microelectronic circuitry, for monitoring transport infrastructure bridges. Such a sensor could provide spatial measurements of strain in excess of 10%. The actual sensor along with the data acquisition module, the communication module and power electronics are all integrated into a compact unit, the SENSKIN device, which is energy-efficient, requires simple signal processing and it is easy to install over various surface types. In terms of communication, SENSKIN devices interact with each other to form the SENSKIN system; a fully distributed and autonomous wireless sensor network that is able to self-monitor. SENSKIN system utilizes Delay-/Disruption-Tolerant Networking technologies to ensure that the strain measurements will be received by the base station even under extreme conditions where normal communications are disrupted. This paper describes the architecture of the SENSKIN system and the development and testing of the first SENSKIN prototype sensor, the data acquisition system, and the communication system.
Y1  - 2017
U6  - https://doi.org/10.1088/1757-899X/236/1/012100
SN  - 1757-8981
VL  - 236
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  -