@article{MarkoetterSintschukBritzkeetal.2022, author = {Mark{\"o}tter, Henning and Sintschuk, Michael and Britzke, Ricardo and Dayani, Shahabeddin and Bruno, Giovanni}, title = {Upgraded imaging capabilities at the BAMline (BESSY II)}, series = {Journal of synchrotron radiation}, volume = {29}, journal = {Journal of synchrotron radiation}, number = {5}, publisher = {International Union of Crystallography}, address = {Chester}, issn = {1600-5775}, doi = {10.1107/S1600577522007342}, pages = {1292 -- 1298}, year = {2022}, abstract = {The BAMline at the BESSY II synchrotron X-ray source has enabled research for more than 20 years in widely spread research fields such as materials science, biology, cultural heritage and medicine. As a nondestructive characterization method, synchrotron X-ray imaging, especially tomography, plays a particularly important role in structural characterization. A recent upgrade of key equipment of the BAMline widens its imaging capabilities: shorter scan acquisition times are now possible, in situ and op erando studies can now be routinely performed, and different energy spectra can easily be set up. In fact, the upgraded double-multilayer monochromator brings full flexibility by yielding different energy spectra to optimize flux and energy resolution as desired. The upgraded detector (based on an sCMOS camera) also allows exploiting the higher flux with reduced readout times. Furthermore, an installed slip ring allows the sample stage to continuously rotate. The latter feature enables tomographic observation of processes occurring in the time scale of a few seconds.}, language = {en} } @article{CestnikMauRosenblum2022, author = {Cestnik, Rok and Mau, Erik T. K. and Rosenblum, Michael}, title = {Inferring oscillator's phase and amplitude response from a scalar signal exploiting test stimulation}, series = {New journal of physics : the open-access journal for physics}, volume = {24}, journal = {New journal of physics : the open-access journal for physics}, number = {12}, publisher = {Dt. Physikalische Ges., IOP}, address = {Bad Honnef, London}, issn = {1367-2630}, doi = {10.1088/1367-2630/aca70a}, pages = {27}, year = {2022}, abstract = {The phase sensitivity curve or phase response curve (PRC) quantifies the oscillator's reaction to stimulation at a specific phase and is a primary characteristic of a self-sustained oscillatory unit. Knowledge of this curve yields a phase dynamics description of the oscillator for arbitrary weak forcing. Similar, though much less studied characteristic, is the amplitude response that can be defined either using an ad hoc approach to amplitude estimation or via the isostable variables. Here, we discuss the problem of the phase and amplitude response inference from observations using test stimulation. Although PRC determination for noise-free neuronal-like oscillators perturbed by narrow pulses is a well-known task, the general case remains a challenging problem. Even more challenging is the inference of the amplitude response. This characteristic is crucial, e.g. for controlling the amplitude of the collective mode in a network of interacting units-a task relevant to neuroscience. Here, we compare the performance of different techniques suitable for inferring the phase and amplitude response, particularly with application to macroscopic oscillators. We suggest improvements to these techniques, e.g. demonstrating how to obtain the PRC in case of stimuli of arbitrary shape. Our main result is a novel technique denoted by IPID-1, based on the direct reconstruction of the Winfree equation and the analogous first-order equation for isostable dynamics. The technique works for signals with or without well-pronounced marker events and pulses of arbitrary shape; in particular, we consider charge-balanced pulses typical in neuroscience applications. Moreover, this technique is superior for noisy and high-dimensional systems. Additionally, we describe an error measure that can be computed solely from data and complements any inference technique.}, language = {en} } @article{DurandvandenBroekeLeCozannetetal.2022, author = {Durand, Gael and van den Broeke, Michiel R. and Le Cozannet, Goneri and Edwards, Tamsin L. and Holland, Paul R. and Jourdain, Nicolas C. and Marzeion, Ben and Mottram, Ruth and Nicholls, Robert J. and Pattyn, Frank and Paul, Frank and Slangen, Aimee B. A. and Winkelmann, Ricarda and Burgard, Clara and van Calcar, Caroline J. and Barre, Jean-Baptiste and Bataille, Amelie and Chapuis, Anne}, title = {Sea-Level rise: from global perspectives to local services}, series = {Frontiers in Marine Science}, volume = {8}, journal = {Frontiers in Marine Science}, publisher = {Frontiers Media}, address = {Lausanne}, issn = {2296-7745}, doi = {10.3389/fmars.2021.709595}, pages = {8}, year = {2022}, abstract = {Coastal areas are highly diverse, ecologically rich, regions of key socio-economic activity, and are particularly sensitive to sea-level change. Over most of the 20th century, global mean sea level has risen mainly due to warming and subsequent expansion of the upper ocean layers as well as the melting of glaciers and ice caps. Over the last three decades, increased mass loss of the Greenland and Antarctic ice sheets has also started to contribute significantly to contemporary sea-level rise. The future mass loss of the two ice sheets, which combined represent a sea-level rise potential of similar to 65 m, constitutes the main source of uncertainty in long-term (centennial to millennial) sea-level rise projections. Improved knowledge of the magnitude and rate of future sea-level change is therefore of utmost importance. Moreover, sea level does not change uniformly across the globe and can differ greatly at both regional and local scales. The most appropriate and feasible sea level mitigation and adaptation measures in coastal regions strongly depend on local land use and associated risk aversion. Here, we advocate that addressing the problem of future sea-level rise and its impacts requires (i) bringing together a transdisciplinary scientific community, from climate and cryospheric scientists to coastal impact specialists, and (ii) interacting closely and iteratively with users and local stakeholders to co-design and co-build coastal climate services, including addressing the high-end risks.}, language = {en} } @article{KretzschmarAshbyFearonetal.2022, author = {Kretzschmar, Mirjam E. and Ashby, Ben and Fearon, Elizabeth and Overton, Christopher E. and Panovska-Griffiths, Jasmina and Pellis, Lorenzo and Quaife, Matthew and Rozhnova, Ganna and Scarabel, Francesca and Stage, Helena B. and Swallow, Ben and Thompson, Robin N. and Tildesley, Michael J. and Villela, Daniel Campos}, title = {Challenges for modelling interventions for future pandemics}, series = {Epidemics}, volume = {38}, journal = {Epidemics}, publisher = {Elsevier}, address = {Amsterdam}, issn = {1755-4365}, doi = {10.1016/j.epidem.2022.100546}, pages = {13}, year = {2022}, abstract = {Mathematical modelling and statistical inference provide a framework to evaluate different non-pharmaceutical and pharmaceutical interventions for the control of epidemics that has been widely used during the COVID-19 pandemic. In this paper, lessons learned from this and previous epidemics are used to highlight the challenges for future pandemic control. We consider the availability and use of data, as well as the need for correct parameterisation and calibration for different model frameworks. We discuss challenges that arise in describing and distinguishing between different interventions, within different modelling structures, and allowing both within and between host dynamics. We also highlight challenges in modelling the health economic and political aspects of interventions. Given the diversity of these challenges, a broad variety of interdisciplinary expertise is needed to address them, combining mathematical knowledge with biological and social insights, and including health economics and communication skills. Addressing these challenges for the future requires strong cross disciplinary collaboration together with close communication between scientists and policy makers.}, language = {en} } @article{AndersKhalatyanQueirozetal.2022, author = {Anders, Friedrich and Khalatyan, Arman and Queiroz, Anna B. A. and Chiappini, Cristina and Ard{\`e}vol, Judith and Casamiquela, Laia and Figueras, Francesca and Jim{\´e}nez-Arranz, {\´O}scar and Jordi, Carme and Monguio, Maria and Romero-G{\´o}mez, Merce and Altamirano, Diego and Antoja, Teresa and Assaad, R. and Cantat-Gaudin, Tristan and Castro-Ginard, Alfred and Enke, Harry and Girardi, L{\´e}o and Guiglion, Guillaume and Khan, Saniya and Luri, Xavier and Miglio, Andrea and Minchev, Ivan and Ramos, Pau and Santiago, Basillio Xavier and Steinmetz, Matthias}, title = {Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia EDR3 stars brighter than G=18.5}, series = {Astronomy and astrophysics}, volume = {658}, journal = {Astronomy and astrophysics}, publisher = {EDP Sciences}, address = {Les Ulis}, issn = {0004-6361}, doi = {10.1051/0004-6361/202142369}, pages = {27}, year = {2022}, abstract = {We present a catalogue of 362 million stellar parameters, distances, and extinctions derived from Gaia's Early Data Release (EDR3) cross-matched with the photometric catalogues of Pan-STARRS1, SkyMapper, 2MASS, and All WISE. The higher precision of the Gaia EDR3 data, combined with the broad wavelength coverage of the additional photometric surveys and the new stellar-density priors of the StarHorse code, allows us to substantially improve the accuracy and precision over previous photo-astrometric stellar-parameter estimates. At magnitude G = 14 (17), our typical precisions amount to 3\% (15\%) in distance, 0.13 mag (0.15 mag) in V-band extinction, and 140 K (180 K) in effective temperature. Our results are validated by comparisons with open clusters, as well as with asteroseismic and spectroscopic measurements, indicating systematic errors smaller than the nominal uncertainties for the vast majority of objects. We also provide distance- and extinction-corrected colour-magnitude diagrams, extinction maps, and extensive stellar density maps that reveal detailed substructures in the Milky Way and beyond. The new density maps now probe a much greater volume, extending to regions beyond the Galactic bar and to Local Group galaxies, with a larger total number density. We publish our results through an ADQL query interface (gaia . aip . de) as well as via tables containing approximations of the full posterior distributions. Our multi-wavelength approach and the deep magnitude limit render our results useful also beyond the next Gaia release, DR3.}, language = {en} } @article{KelesMallonnKitzmannetal.2022, author = {Keles, Engin and Mallonn, Matthias and Kitzmann, Daniel and Poppenh{\"a}ger, Katja and Hoeijmakers, H. Jens and Ilyin, Ilya and Alexoudi, Xanthippi and Carroll, Thorsten A. and Alvarado-Gomez, Julian and Ketzer, Laura and Bonomo, Aldo S. and Borsa, Francesco and Gaudi, B. Scott and Henning, Thomas and Malavolta, Luca and Molaverdikhani, Karan and Nascimbeni, Valerio and Patience, Jennifer and Pino, Lorenzo and Scandariato, Gaetano and Schlawin, Everett and Shkolnik, Evgenya and Sicilia, Daniela and Sozzetti, Alessandro and Foster, Mary G. and Veillet, Christian and Wang, Ji and Yan, Fei and Strassmeier, Klaus G.}, title = {The PEPSI exoplanet transit survey (PETS) I: Investigating the presence of a silicate atmosphere on the super-earth 55 Cnc e}, series = {Monthly notices of the Royal Astronomical Society}, volume = {513}, journal = {Monthly notices of the Royal Astronomical Society}, number = {1}, publisher = {Oxford University Press}, address = {Oxford}, issn = {0035-8711}, doi = {10.1093/mnras/stac810}, pages = {1544 -- 1556}, year = {2022}, abstract = {The study of exoplanets and especially their atmospheres can reveal key insights on their evolution by identifying specific atmospheric species. For such atmospheric investigations, high-resolution transmission spectroscopy has shown great success, especially for Jupiter-type planets. Towards the atmospheric characterization of smaller planets, the super-Earth exoplanet 55 Cnc e is one of the most promising terrestrial exoplanets studied to date. Here, we present a high-resolution spectroscopic transit observation of this planet, acquired with the PEPSI instrument at the Large Binocular Telescope. Assuming the presence of Earth-like crust species on the surface of 55 Cnc e, from which a possible silicate-vapor atmosphere could have originated, we search in its transmission spectrum for absorption of various atomic and ionized species such as Fe , Fe (+), Ca , Ca (+), Mg, and K , among others. Not finding absorption for any of the investigated species, we are able to set absorption limits with a median value of 1.9 x R-P. In conclusion, we do not find evidence of a widely extended silicate envelope on this super-Earth reaching several planetary radii.}, language = {en} } @article{KramerBouriaudFeindtetal.2022, author = {Kramer, Koen and Bouriaud, Laura and Feindt, Peter H. and van Wassenaer, Lan and Glanemann, Nicole and Hanewinkel, Marc and van der Heide, Martijn and Hengeveld, Geerten M. and Hoogstra, Marjanke and Ingram, Verina and Levermann, Anders and Lindner, Marcus and M{\´a}ty{\´a}s, Csaba and Mohren, Frits and Muys, Bart and Nabuurs, Gert-Jan and Palahi, Marc and Polman, Nico and Reyer, Christopher P. O. and Schulze, Ernst-Detlef and Seidl, Rupert and de Vries, Wim and Werners, Saskia E. and Winkel, Georg and Yousefpour, Rasoul}, title = {Perspective Roadmap to develop a stress test for forest ecosystem services supply}, series = {One Earth}, volume = {5}, journal = {One Earth}, number = {1}, publisher = {Elsevier}, address = {Amsterdam}, issn = {2590-3330}, doi = {10.1016/j.oneear.2021.12.009}, pages = {25 -- 34}, year = {2022}, abstract = {Forests play a key role in a bio-based economy by providing renewable materials, mitigating climate change, and accommodating biodiversity. However, forests experience massive increases in stresses in their ecological and socioeconomic environments, threatening forest ecosystem services supply. Alleviating those stresses is hampered by conflicting and disconnected governance arrangements, competing interests and claims, and rapid changes in technology and social demands. Identifying which stresses threaten forest ecosystem services supply and which factors hamper their alleviation requires stakeholders' perceptions. Stakeholder-oriented stress tests for the supply of forest ecosystem services are therefore necessary but are not yet available. This perspective presents a roadmap to develop a stress test tailored to multiple stakeholders' needs and demands across spatial scales. We provide the Cascade and Resilience Rosetta, with accompanying performance- and resilience indicators, as tools to facilitate development of the stress test. The application of the stress test will facilitate the transition toward a bio-based economy in which healthy and diverse forests provide sustainable and resilient ecosystem services.}, language = {en} } @article{HempelSavenjieStolterfohtetal.2022, author = {Hempel, Hannes and Savenjie, Tom J. and Stolterfoht, Martin and Neu, Jens and Failla, Michele and Paingad, Vaisakh C. and Kužel, Petr and Heilweil, Edwin J. and Spies, Jacob A. and Schleuning, Markus and Zhao, Jiashang and Friedrich, Dennis and Schwarzburg, Klaus and Siebbeles, Laurens D. A. and D{\"o}rflinger, Patrick and Dyakonov, Vladimir and Katoh, Ryuzi and Hong, Min Ji and Labram, John G. and Monti, Maurizio and Butler-Caddle, Edward and Lloyd-Hughes, James and Taheri, Mohammad M. and Baxter, Jason B. and Magnanelli, Timothy J. and Luo, Simon and Cardon, Joseph M. and Ardo, Shane and Unold, Thomas}, title = {Predicting solar cell performance from terahertz and microwave spectroscopy}, series = {Advanced energy materials}, volume = {12}, journal = {Advanced energy materials}, number = {13}, publisher = {Wiley}, address = {Weinheim}, issn = {1614-6832}, doi = {10.1002/aenm.202102776}, pages = {16}, year = {2022}, abstract = {Mobilities and lifetimes of photogenerated charge carriers are core properties of photovoltaic materials and can both be characterized by contactless terahertz or microwave measurements. Here, the expertise from fifteen laboratories is combined to quantitatively model the current-voltage characteristics of a solar cell from such measurements. To this end, the impact of measurement conditions, alternate interpretations, and experimental inter-laboratory variations are discussed using a (Cs,FA,MA)Pb(I,Br)(3) halide perovskite thin-film as a case study. At 1 sun equivalent excitation, neither transport nor recombination is significantly affected by exciton formation or trapping. Terahertz, microwave, and photoluminescence transients for the neat material yield consistent effective lifetimes implying a resistance-free JV-curve with a potential power conversion efficiency of 24.6 \%. For grainsizes above approximate to 20 nm, intra-grain charge transport is characterized by terahertz sum mobilities of approximate to 32 cm(2) V-1 s(-1). Drift-diffusion simulations indicate that these intra-grain mobilities can slightly reduce the fill factor of perovskite solar cells to 0.82, in accordance with the best-realized devices in the literature. Beyond perovskites, this work can guide a highly predictive characterization of any emerging semiconductor for photovoltaic or photoelectrochemical energy conversion. A best practice for the interpretation of terahertz and microwave measurements on photovoltaic materials is presented.}, language = {en} } @article{HuthPangTewsetal.2022, author = {Huth, Sabrina and Pang, Peter Tsun Ho and Tews, Ingo and Dietrich, Tim and Le F{\`e}vre, Arnaud and Schwenk, Achim and Trautmann, Wolfgang and Agarwal, Kshitij and Bulla, Mattia and Coughlin, Michael W. and Van den Broeck, Chris}, title = {Constraining neutron-star matter with microscopic and macroscopic collisions}, series = {Nature : the international weekly journal of science}, volume = {606}, journal = {Nature : the international weekly journal of science}, number = {7913}, publisher = {Nature Publ. Group}, address = {London [u.a.]}, issn = {0028-0836}, doi = {10.1038/s41586-022-04750-w}, pages = {276 -- 295}, year = {2022}, abstract = {Interpreting high-energy, astrophysical phenomena, such as supernova explosions or neutron-star collisions, requires a robust understanding of matter at supranuclear densities. However, our knowledge about dense matter explored in the cores of neutron stars remains limited. Fortunately, dense matter is not probed only in astrophysical observations, but also in terrestrial heavy-ion collision experiments. Here we use Bayesian inference to combine data from astrophysical multi-messenger observations of neutron stars(1-9) and from heavy-ion collisions of gold nuclei at relativistic energies(10,11) with microscopic nuclear theory calculations(12-17) to improve our understanding of dense matter. We find that the inclusion of heavy-ion collision data indicates an increase in the pressure in dense matter relative to previous analyses, shifting neutron-star radii towards larger values, consistent with recent observations by the Neutron Star Interior Composition Explorer mission(5-8,18). Our findings show that constraints from heavy-ion collision experiments show a remarkable consistency with multi-messenger observations and provide complementary information on nuclear matter at intermediate densities. This work combines nuclear theory, nuclear experiment and astrophysical observations, and shows how joint analyses can shed light on the properties of neutron-rich supranuclear matter over the density range probed in neutron stars.}, language = {en} } @article{PetrovSingerCoughlinetal.2022, author = {Petrov, Polina and Singer, Leo P. and Coughlin, Michael W. and Kumar, Vishwesh and Almualla, Mouza and Anand, Shreya and Bulla, Mattia and Dietrich, Tim and Foucart, Francois and Guessoum, Nidhal}, title = {Data-driven expectations for electromagnetic counterpart searches based on LIGO/Virgo public alerts}, series = {The astrophysical journal : an international review of spectroscopy and astronomical physics; part 1}, volume = {924}, journal = {The astrophysical journal : an international review of spectroscopy and astronomical physics; part 1}, number = {2}, publisher = {Institute of Physics Publ.}, address = {London}, issn = {1538-4357}, doi = {10.3847/1538-4357/ac366d}, pages = {10}, year = {2022}, abstract = {Searches for electromagnetic counterparts of gravitational-wave signals have redoubled since the first detection in 2017 of a binary neutron star merger with a gamma-ray burst, optical/infrared kilonova, and panchromatic afterglow. Yet, one LIGO/Virgo observing run later, there has not yet been a second, secure identification of an electromagnetic counterpart. This is not surprising given that the localization uncertainties of events in LIGO and Virgo's third observing run, O3, were much larger than predicted. We explain this by showing that improvements in data analysis that now allow LIGO/Virgo to detect weaker and hence more poorly localized events have increased the overall number of detections, of which well-localized, gold-plated events make up a smaller proportion overall. We present simulations of the next two LIGO/Virgo/KAGRA observing runs, O4 and O5, that are grounded in the statistics of O3 public alerts. To illustrate the significant impact that the updated predictions can have, we study the follow-up strategy for the Zwicky Transient Facility. Realistic and timely forecasting of gravitational-wave localization accuracy is paramount given the large commitments of telescope time and the need to prioritize which events are followed up. We include a data release of our simulated localizations as a public proposal planning resource for astronomers.}, language = {en} } @article{KollmannRoussosClarketal.2022, author = {Kollmann, Peter and Roussos, Elias and Clark, George and Cooper, John F. and Sturner, Steven J. and Kotova, Anna and Regoli, Leonardo and Shprits, Yuri and Aseev, Nikita and Krupp, Norbert}, title = {Spectra of Saturn's proton belts revealed}, series = {Icarus}, volume = {376}, journal = {Icarus}, publisher = {Elsevier}, address = {San Diego}, issn = {0019-1035}, doi = {10.1016/j.icarus.2021.114795}, pages = {17}, year = {2022}, abstract = {Saturn is permanently surrounded by 6 discrete proton radiation belts that are rigidly separated by the orbits of its inner moons and dense rings. These radiation belts are ideal environments to study the details of radial diffusion and the CRAND source process, yet progress has been hindered by the fact that the energy spectra are not known with certainty: Reanalysis of the response functions of the LEMMS instrument on-board the Cassini orbiter has shown that measurements of less than or similar to 10 MeV protons may be easily contaminated by greater than or similar to 10 MeV protons and that many available measurements characterize a very broad energy range, so that the calculation of an energy-resolved spectrum is not as straightforward as previously assumed. Here we use forward modeling of the measurements based on the instrument response and combine this technique where useful with numerical modeling of the proton belt physics in order to determine Saturn's spectra with higher certainty. We find significant proton intensities up to approximate to 1 GeV. While earlier studies reported on proton spectra roughly following a power law with exponent approximate to -2, our more advanced analysis shows harder spectra with exponent approximate to -1. The observed spectra provide independent confirmation that Saturn's proton belts are sourced by CRAND and are consistent with the provided protons being subsequently cooled in the tenuous gas originating from Saturn or Enceladus. The intensities at Saturn are found to be lower than at Jupiter and Earth, which is also consistent with the source of Saturn being exclusively CRAND, while the other planets can draw from additional processes. Our new spectra can be used in the future to further our understanding of Saturn's proton belts and the respective physical processes that occur at other magnetized planets in general. Also, the spectra have applications for several topics of planetary science, such as space weathering of Saturn's moons and rings, and can be useful to constrain properties of the main rings through their production of secondary particles.}, language = {en} } @article{SchaererIzotovWorsecketal.2022, author = {Schaerer, Daniel and Izotov, Yuri I. and Worseck, G{\´a}bor and Berg, Danielle and Chisholm, John and Jaskot, Anne and Nakajima, Kimihiko and Ravindranath, Swara and Thuan, Trinh X. and Verhamme, Anne}, title = {Strong Lyman continuum emitting galaxies show intense C IV λ 1550 emission}, series = {Astronomy and astrophysics}, volume = {658}, journal = {Astronomy and astrophysics}, publisher = {EDP Sciences}, address = {Les Ulis}, issn = {0004-6361}, doi = {10.1051/0004-6361/202243149}, pages = {6}, year = {2022}, abstract = {Using the Space Telescope Imaging Spectrograph, we have obtained ultraviolet spectra from similar to 1200 to 2000 angstrom of known Lyman continuum (LyC) emitting galaxies at low redshift (z similar to 0.3-0.4) with varying absolute LyC escape fractions ( f(esc) similar to 0.01-0.72). Our observations include in particular the galaxy J1243+4646, which has the highest known LyC escape fraction at low redshift. While all galaxies are known Lyman alpha emitters, we consistently detect an inventory of additional emission lines, including C IV lambda 1550, He II lambda 1640, O III] lambda 1666, and C III] lambda 1909, whose origin is presumably essentially nebular. C IV lambda 1550 emission is detected above 4 sigma in six out of eight galaxies, with equivalent widths of EW(C IV) = 12-15 angstrom for two galaxies, which exceeds the previously reported maximum emission in low-z star-forming galaxies. We detect C IV lambda 1550 emission in all LyC emitters with escape fractions f(esc) > 0.1 and find a tentative increase in the flux ratio C IV lambda 1550 /C III] lambda 1909 with f(esc). Based on the data, we propose a new criterion to select and classify strong leakers (galaxies with f(esc) > 0.1): C IV lambda 1550 /C III] lambda 1909 greater than or similar to 0.75. Finally, we also find He II lambda 1640 emission in all the strong leakers with equivalent widths from 3 to 8 angstrom rest frame. These are among the highest values observed in star-forming galaxies and are primarily due to a high rate of ionizing photon production. The nebular He II lambda 1640 emission of the strong LyC emitters does not require harder ionizing spectra at >54 eV compared to those of typical star-forming galaxies at similarly low metallicity.}, language = {en} } @article{CiarnielloFulleRaponietal.2022, author = {Ciarniello, Mauro and Fulle, Marco and Raponi, Andrea and Filacchione, Gianrico and Capaccioni, Fabrizio and Rotundi, Alessandra and Rinaldi, Giovanna and Formisano, Michelangelo and Magni, Gianfranco and Tosi, Federico and De Sanctis, Maria Cristina and Capria, Maria Teresa and Longobardo, Andrea and Beck, Pierre and Fornasier, Sonia and Kappel, David and Mennella, Vito and Mottola, Stefano and Rousseau, Batiste and Arnold, Gabriele}, title = {Macro and micro structures of pebble-made cometary nuclei reconciled by seasonal evolution}, series = {Nature astronomy}, volume = {6}, journal = {Nature astronomy}, number = {5}, publisher = {Nature Research}, address = {Berlin}, issn = {2397-3366}, doi = {10.1038/s41550-022-01625-y}, pages = {546 -- 553}, year = {2022}, abstract = {Comets evolve due to sublimation of ices embedded inside porous dust, triggering dust emission (that is, erosion) followed by mass loss, mass redistribution and surface modifications. Surface changes were revealed by the Deep Impact and Stardust NExT missions for comet 9P/Tempel 1 (ref.(1)), and a full inventory of the processes modifying cometary nuclei was provided by Rosetta while it escorted comet 67P/Churyumov-Gerasimenko for approximately two years(2-4). Such observations also showed puzzling water-ice-rich spots that stood out as patches optically brighter and spectrally bluer than the average cometary surfaces(5-9). These are up to tens of metres large and indicate macroscopic compositional dishomogeneities apparently in contrast with the structural homogeneity above centimetre scales of pebble-made nuclei(10). Here we show that the occurrence of blue patches determines the seasonal variability of the nucleus colour(4,11,12) and gives insight into the internal structure of comets. We define a new model that links the centimetre-sized pebbles composing the nucleus(10) and driving cometary activity(13,14) to metre-sized water-ice-enriched blocks embedded in a drier matrix. The emergence of blue patches is due to the matrix erosion driven by CO2-ice sublimation that exposes the water-ice-enriched blocks, which in turn are eroded by water-ice sublimation when exposed to sunlight. Our model explains the observed seasonal evolution of the nucleus and reconciles the available data at micro (sub-centimetre) and macro (metre) scales.}, language = {en} } @article{KupferBauervanRoesteletal.2022, author = {Kupfer, Thomas and Bauer, Evan B. and van Roestel, Jan and Bellm, Eric C. and Bildsten, Lars and Fuller, Jim and Prince, Thomas A. and Heber, Ulrich and Geier, Stephan and Green, Matthew J. and Kulkarni, Shrinivas R. and Bloemen, Steven and Laher, Russ R. and Rusholme, Ben and Schneider, David}, title = {Discovery of a Double-detonation Thermonuclear Supernova Progenitor}, series = {The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters}, volume = {925}, journal = {The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters}, number = {2}, publisher = {IOP Publ. Ltd.}, address = {Bristol}, issn = {2041-8205}, doi = {10.3847/2041-8213/ac48f1}, pages = {10}, year = {2022}, abstract = {We present the discovery of a new double-detonation progenitor system consisting of a hot subdwarf B (sdB) binary with a white dwarf companion with a P (orb) = 76.34179(2) minutes orbital period. Spectroscopic observations are consistent with an sdB star during helium core burning residing on the extreme horizontal branch. Chimera light curves are dominated by ellipsoidal deformation of the sdB star and a weak eclipse of the companion white dwarf. Combining spectroscopic and light curve fits, we find a low-mass sdB star, M (sdB) = 0.383 +/- 0.028 M (circle dot) with a massive white dwarf companion, M (WD) = 0.725 +/- 0.026 M (circle dot). From the eclipses we find a blackbody temperature for the white dwarf of 26,800 K resulting in a cooling age of approximate to 25 Myr whereas our MESA model predicts an sdB age of approximate to 170 Myr. We conclude that the sdB formed first through stable mass transfer followed by a common envelope which led to the formation of the white dwarf companion approximate to 25 Myr ago. Using the MESA stellar evolutionary code we find that the sdB star will start mass transfer in approximate to 6 Myr and in approximate to 60 Myr the white dwarf will reach a total mass of 0.92 M (circle dot) with a thick helium layer of 0.17 M (circle dot). This will lead to a detonation that will likely destroy the white dwarf in a peculiar thermonuclear supernova. PTF1 J2238+7430 is only the second confirmed candidate for a double-detonation thermonuclear supernova. Using both systems we estimate that at least approximate to 1\% of white dwarf thermonuclear supernovae originate from sdB+WD binaries with thick helium layers, consistent with the small number of observed peculiar thermonuclear explosions.}, language = {en} } @article{SchwopePiresKurpasetal.2022, author = {Schwope, Axel and Pires, Adriana M. and Kurpas, Jan and Doroshenko, Victor and Suleimanov, Valery F. and Freyberg, Michael and Becker, Werner and Dennerl, Konrad and Haberl, Frank and Lamer, Georg and Maitra, Chandreyee and Potekhin, Alexander Y. and Ramos-Ceja, Miriam E. and Santangelo, Andrea and Traulsen, Iris and Werner, Klaus}, title = {Phase-resolved X-ray spectroscopy of PSR B0656+14 with SRG/eROSITA and XMM-Newton}, series = {Astronomy and astrophysics : an international weekly journal}, volume = {661}, journal = {Astronomy and astrophysics : an international weekly journal}, publisher = {EDP Sciences}, address = {Les Ulis}, issn = {0004-6361}, doi = {10.1051/0004-6361/202141105}, pages = {21}, year = {2022}, abstract = {We present a detailed spectroscopic and timing analysis of X-ray observations of the bright pulsar PSR B0656+14. The observations were obtained simultaneously with eROSITA and XMM-Newton during the calibration and performance verification phase of the Spektrum-Roentgen-Gamma mission (SRG). The analysis of the 100 ks deep observation of eROSITA is supported by archival observations of the source, including XMM-Newton, NuSTAR, and NICER. Using XMM-Newton and NICER, we first established an X-ray ephemeris for the time interval 2015 to 2020, which connects all X-ray observations in this period without cycle count alias and phase shifts. The mean eROSITA spectrum clearly reveals an absorption feature originating from the star at 570 eV with a Gaussian sigma of about 70 eV that was tentatively identified in a previous long XMM-Newton observation. A second previously discussed absorption feature occurs at 260-265 eV and is described here as an absorption edge. It could be of atmospheric or of instrumental origin. These absorption features are superposed on various emission components that are phenomenologically described here as the sum of hot (120 eV) and cold (65 eV) blackbody components, both of photospheric origin, and a power law with photon index Gamma = 2 from the magnetosphere. We created energy-dependent light curves and phase-resolved spectra with a high signal-to-noise ratio. The phase-resolved spectroscopy reveals that the Gaussian absorption line at 570 eV is clearly present throughout similar to 60\% of the spin cycle, but it is otherwise undetected. Likewise, its parameters were found to be dependent on phase. The visibility of the line strength coincides in phase with the maximum flux of the hot blackbody. If the line originates from the stellar surface, it nevertheless likely originates from a different location than the hot polar cap. We also present three families of model atmospheres: a magnetized atmosphere, a condensed surface, and a mixed model. They were applied to the mean observed spectrum, whose continuum fit the observed data well. The atmosphere model, however, predicts distances that are too short. For the mixed model, the Gaussian absorption may be interpreted as proton cyclotron absorption in a field as high as 10(14) G, which is significantly higher than the field derived from the moderate observed spin-down.}, language = {en} } @article{WarbyZuZeiskeetal.2022, author = {Warby, Jonathan and Zu, Fengshuo and Zeiske, Stefan and Gutierrez-Partida, Emilio and Frohloff, Lennart and Kahmann, Simon and Frohna, Kyle and Mosconi, Edoardo and Radicchi, Eros and Lang, Felix and Shah, Sahil and Pena-Camargo, Francisco and Hempel, Hannes and Unold, Thomas and Koch, Norbert and Armin, Ardalan and De Angelis, Filippo and Stranks, Samuel D. and Neher, Dieter and Stolterfoht, Martin}, title = {Understanding performance limiting interfacial recombination in pin Perovskite solar cells}, series = {Advanced energy materials}, volume = {12}, journal = {Advanced energy materials}, number = {12}, publisher = {Wiley-VCH}, address = {Weinheim}, issn = {1614-6832}, doi = {10.1002/aenm.202103567}, pages = {10}, year = {2022}, abstract = {Perovskite semiconductors are an attractive option to overcome the limitations of established silicon based photovoltaic (PV) technologies due to their exceptional opto-electronic properties and their successful integration into multijunction cells. However, the performance of single- and multijunction cells is largely limited by significant nonradiative recombination at the perovskite/organic electron transport layer junctions. In this work, the cause of interfacial recombination at the perovskite/C-60 interface is revealed via a combination of photoluminescence, photoelectron spectroscopy, and first-principle numerical simulations. It is found that the most significant contribution to the total C-60-induced recombination loss occurs within the first monolayer of C-60, rather than in the bulk of C-60 or at the perovskite surface. The experiments show that the C-60 molecules act as deep trap states when in direct contact with the perovskite. It is further demonstrated that by reducing the surface coverage of C-60, the radiative efficiency of the bare perovskite layer can be retained. The findings of this work pave the way toward overcoming one of the most critical remaining performance losses in perovskite solar cells.}, language = {en} } @article{HerbstBaalmannBykovetal.2022, author = {Herbst, Konstantin and Baalmann, Lennart R. and Bykov, Andrei and Engelbrecht, N. Eugene and Ferreira, Stefan E. S. and Izmodenov, Vladislav V. and Korolkov, Sergey D. and Levenfish, Ksenia P. and Linsky, Jeffrey L. and Meyer, Dominique M. -A. and Scherer, Klaus and Strauss, R. Du Toit}, title = {Astrospheres of planet-hosting cool stars and beyond when modeling meets observations}, series = {Space science reviews}, volume = {218}, journal = {Space science reviews}, number = {4}, publisher = {Springer Nature}, address = {Dordrecht}, issn = {0038-6308}, doi = {10.1007/s11214-022-00894-3}, pages = {46}, year = {2022}, abstract = {Thanks to dedicated long-term missions like Voyager and GOES over the past 50 years, much insight has been gained on the activity of our Sun, the solar wind, its interaction with the interstellar medium, and, thus, about the formation, the evolution, and the structure of the heliosphere. Additionally, with the help of multi-wavelength observations by the Hubble Space Telescope, Kepler, and TESS, we not only were able to detect a variety of extrasolar planets and exomoons but also to study the characteristics of their host stars, and thus became aware that other stars drive bow shocks and astrospheres. Although features like, e.g., stellar winds, could not be measured directly, over the past years several techniques have been developed allowing us to indirectly derive properties like stellar mass-loss rates and stellar wind speeds, information that can be used as direct input to existing astrospheric modeling codes. In this review, the astrospheric modeling efforts of various stars will be presented. Starting with the heliosphere as a benchmark of astrospheric studies, investigating the paleo-heliospheric changes and the Balmer H alpha projections to 1 pc, we investigate the surroundings of cool and hot stars, but also of more exotic objects like neutron stars. While pulsar wind nebulae (PWNs) might be a source of high-energy galactic cosmic rays (GCRs), the astrospheric environments of cool and hot stars form a natural shield against GCRs. Their modulation within these astrospheres, and the possible impact of turbulence, are also addressed. This review shows that all of the presented modeling efforts are in excellent agreement with currently available observations.}, language = {en} } @article{OranWeissSantacruzPichetal.2022, author = {Oran, Rona and Weiss, Benjamin P. and Santacruz-Pich, Maria De Soria and Jun, Insoo and Lawrence, David J. and Polanskey, Carol A. and Ratliff, J. Martin and Raymond, Carol A. and Ream, Jodie B. and Russell, Christopher T. and Shprits, Yuri and Zuber, Maria T. and Elkins-Tanton, Linda T.}, title = {Maximum energies of trapped particles around magnetized planets and small bodies}, series = {Geophysical research letters}, volume = {49}, journal = {Geophysical research letters}, number = {13}, publisher = {American Geophysical Union}, address = {Washington}, issn = {0094-8276}, doi = {10.1029/2021GL097014}, pages = {11}, year = {2022}, abstract = {Energetic charged particles trapped in planetary radiation belts are hazardous to spacecraft. Planned missions to iron-rich asteroids with possible strong remanent magnetic fields require an assessment of trapped particles energies. Using laboratory measurements of iron meteorites, we estimate the largest possible asteroid magnetic moment. Although weak compared to moments of planetary dynamos, the small body size may yield strong surface fields. We use hybrid simulations to confirm the formation of a magnetosphere with an extended quasi-dipolar region. However, the short length scale of the field implies that energetic particle motion would be nonadiabatic, making existing radiation belt theories not applicable. Our idealized particle simulations demonstrate that chaotic motions lead to particle loss at lower energies than those predicted by adiabatic theory, which may explain the energies of transiently trapped particles observed at Mercury, Ganymede, and Earth. However, even the most magnetized asteroids are unlikely to stably trap hazardous particles.}, language = {en} } @article{AguileraDenaLangerAntoniadisetal.2022, author = {Aguilera-Dena, David R. and Langer, Norbert and Antoniadis, John and Pauli, Daniel and Dessart, Luc and Vigna-G{\´o}mez, Alejandro and Gr{\"a}fener, G{\"o}tz and Yoon, Sung-Chul}, title = {Stripped-envelope stars in different metallicity environments: I. Evolutionary phases, classification, and populations}, series = {Astronomy and astrophysics}, volume = {661}, journal = {Astronomy and astrophysics}, publisher = {EDP Sciences}, address = {Les Ulis}, issn = {0004-6361}, doi = {10.1051/0004-6361/202142895}, pages = {20}, year = {2022}, abstract = {Massive stars that become stripped of their hydrogen envelope through binary interaction or winds can be observed either as Wolf-Rayet stars, if they have optically thick winds, or as transparent-wind stripped-envelope stars. We approximate their evolution through evolutionary models of single helium stars, and compute detailed model grids in the initial mass range 1.5-70 M. for metallicities between 0.01 and 0.04, from core helium ignition until core collapse. Throughout their lifetimes some stellar models expose the ash of helium burning. We propose that models that have nitrogen-rich envelopes are candidate WN stars, while models with a carbon-rich surface are candidate WC stars during core helium burning, and WO stars afterwards. We measure the metallicity dependence of the total lifetimes of our models and the duration of their evolutionary phases. We propose an analytic estimate of the wind's optical depth to distinguish models of Wolf-Rayet stars from transparent-wind stripped-envelope stars, and find that the luminosity ranges at which WN-, WC-, and WO-type stars can exist is a strong function of metallicity. We find that all carbon-rich models produced in our grids have optically thick winds and match the luminosity distribution of observed populations. We construct population models and predict the numbers of transparent-wind stripped-envelope stars and Wolf-Rayet stars, and derive their number ratios at different metallicities. We find that as metallicity increases, the number of transparent-wind stripped-envelope stars decreases and the number of Wolf-Rayet stars increases. At high metallicities WC- and WO-type stars become more common. We apply our population models to nearby galaxies, and find that populations are more sensitive to the transition luminosity between Wolf-Rayet stars and transparent-wind helium stars than to the metallicity-dependent mass loss rates.}, language = {en} } @article{MarinBeloquiZhangGuoetal.2022, author = {Marin-Beloqui, Jose and Zhang, Guanran and Guo, Junjun and Shaikh, Jordan and Wohrer, Thibaut and Hosseini, Seyed Mehrdad and Sun, Bowen and Shipp, James and Auty, Alexander J. and Chekulaev, Dimitri and Ye, Jun and Chin, Yi-Chun and Sullivan, Michael B. and Mozer, Attila J. and Kim, Ji-Seon and Shoaee, Safa and Clarke, Tracey M.}, title = {Insight into the origin of trapping in polymer/fullerene blends with a systematic alteration of the fullerene to higher adducts}, series = {Journal of physical chemistry C}, volume = {126}, journal = {Journal of physical chemistry C}, number = {5}, publisher = {American Chemical Society}, address = {Washington}, issn = {1932-7447}, doi = {10.1021/acs.jpcc.1c10378}, pages = {2708 -- 2719}, year = {2022}, abstract = {The bimolecular recombination characteristics of conjugated polymer poly[(4,4'-bis(2-ethylhexyl)dithieno[3,2-b:2',3'-d]silole)-2,6-diyl-alt-(2,5-bis 3-tetradecylthiophen-2-y1 thiazolo 5,4-d thiazole)-2,5diy1] (PDTSiTTz) blended with the fullerene series PC60BM, ICMA, ICBA, and ICTA have been investigated using microsecond and femtosecond transient absorption spectroscopy, in conjunction with electroluminescence measurements and ambient photoemission spectroscopy. The non-Langevin polymer PDTSiTTz allows an inspection of intrinsic bimolecular recombination rates uninhibited by diffusion, while the low oscillator strengths of fullerenes allow polymer features to dominate, and we compare our results to those of the well-known polymer Si-PCPDTBT. Using mu s-TAS, we have shown that the trap -limited decay dynamics of the PDTSiTTz polaron becomes progressively slower across the fullerene series, while those of Si-PCPDTBT are invariant. Electroluminescence measurements showed an unusual double peak in pristine PDTSiTTz, attributed to a low energy intragap charge transfer state, likely interchain in nature. Furthermore, while the pristine PDTSiTTz showed a broad, low-intensity density of states, the ICBA and ICTA blends presented a virtually identical DOS to Si-PCPDTBT and its blends. This has been attributed to a shift from a delocalized, interchain highest occupied molecular orbital (HOMO) in the pristine material to a dithienosilole-centered HOMO in the blends, likely a result of the bulky fullerenes increasing interchain separation. This HOMO localization had a side effect of progressively shifting the polymer HOMO to shallower energies, which was correlated with the observed decrease in bimolecular recombination rate and increased "trap" depth. However, since the density of tail states remained the same, this suggests that the traditional viewpoint of "trapping" being dominated by tail states may not encompass the full picture and that the breadth of the DOS may also have a strong influence on bimolecular recombination.}, language = {en} }