TY - JOUR A1 - Kupfer, Thomas A1 - Bauer, Evan B. A1 - van Roestel, Jan A1 - Bellm, Eric C. A1 - Bildsten, Lars A1 - Fuller, Jim A1 - Prince, Thomas A. A1 - Heber, Ulrich A1 - Geier, Stephan A1 - Green, Matthew J. A1 - Kulkarni, Shrinivas R. A1 - Bloemen, Steven A1 - Laher, Russ R. A1 - Rusholme, Ben A1 - Schneider, David T1 - Discovery of a Double-detonation Thermonuclear Supernova Progenitor JF - The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters N2 - 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. Y1 - 2022 U6 - https://doi.org/10.3847/2041-8213/ac48f1 SN - 2041-8205 SN - 2041-8213 VL - 925 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Jaiser, Ralf A1 - Akperov, Mirseid A1 - Timazhev, A. A1 - Romanowsky, Erik A1 - Handorf, Dörthe A1 - Mokhov, I. I. T1 - Linkages between arctic and mid-latitude weather and climate BT - unraveling the impact of changing sea ice and sea surface temperatures during Winter JF - Meteorologische Zeitschrift N2 - The study addresses the question, if observed changes in terms of Arctic-midlatitude linkages during winter are driven by Arctic Sea ice decline alone or if the increase of global sea surface temperatures plays an additional role. We compare atmosphere-only model experiments with ECHAM6 to ERA-Interim Reanalysis data. The model sensitivity experiment is implemented as a set of four combinations of sea ice and sea surface temperature boundary conditions. Atmospheric circulation regimes are determined and evaluated in terms of their cyclone and blocking characteristics and changes in frequency during winter. As a prerequisite, ECHAM6 reproduces general features of circulation regimes very well. Tropospheric changes induced by the change of boundary conditions are revealed and further impacts on the large-scale circulation up into the stratosphere are investigated. In early winter, the observed increase of atmospheric blocking in the region between Scandinavia and the Urals are primarily related to the changes in sea surface temperatures. During late winter, we f nd a weakened polar stratospheric vortex in the reanalysis that further impacts the troposphere. In the model sensitivity study a climatologically weakened polar vortex occurs only if sea ice is reduced and sea surface temperatures are increased together. This response is delayed compared to the reanalysis. The tropospheric response during late winter is inconclusive in the model, which is potentially related to the weak and delayed response in the stratosphere. The model experiments do not reproduce the connection between early and late winter as interpreted from the reanalysis. Potentially explaining this mismatch, we identify a discrepancy of ECHAM6 to reproduce the weakening of the stratospheric polar vortex through blocking induced upward propagation of planetary waves. KW - Weather regimes KW - Blocking KW - Cyclones KW - Wave Propagation KW - Stratosphere Y1 - 2023 U6 - https://doi.org/10.1127/metz/2023/1154 SN - 0941-2948 SN - 1610-1227 VL - 32 IS - 3 SP - 173 EP - 194 PB - Schweizerbart CY - Stuttgart ER - TY - JOUR A1 - Di Bello, Costantino A1 - Hartmann, Alexander K. A1 - Majumdar, Satya N. A1 - Mori, Francesco A1 - Rosso, Alberto A1 - Schehr, Gregory T1 - Current fluctuations in stochastically resetting particle systems JF - Physical review : E, Statistical, nonlinear and soft matter physics N2 - We consider a system of noninteracting particles on a line with initial positions distributed uniformly with density ? on the negative half-line. We consider two different models: (i) Each particle performs independent Brownian motion with stochastic resetting to its initial position with rate r and (ii) each particle performs run -and-tumble motion, and with rate r its position gets reset to its initial value and simultaneously its velocity gets randomized. We study the effects of resetting on the distribution P(Q, t) of the integrated particle current Q up to time t through the origin (from left to right). We study both the annealed and the quenched current distributions and in both cases, we find that resetting induces a stationary limiting distribution of the current at long times. However, we show that the approach to the stationary state of the current distribution in the annealed and the quenched cases are drastically different for both models. In the annealed case, the whole distribution P-an(Q, t) approaches its stationary limit uniformly for all Q. In contrast, the quenched distribution P-qu(Q, t) attains its stationary form for Q < Q(crit)(t), while it remains time dependent for Q > Q(crit)(t). We show that Q(crit)(t) increases linearly with t for large t. On the scale where Q <; Q(crit)(t), we show that P-qu(Q, t) has an unusual large deviation form with a rate function that has a third-order phase transition at the critical point. We have computed the associated rate functions analytically for both models. Using an importance sampling method that allows to probe probabilities as tiny as 10-14000, we were able to compute numerically this nonanalytic rate function for the resetting Brownian dynamics and found excellent agreement with our analytical prediction. Y1 - 2023 U6 - https://doi.org/10.1103/PhysRevE.108.014112 SN - 2470-0045 SN - 2470-0053 VL - 108 IS - 1 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Schwope, Axel A1 - Pires, Adriana M. A1 - Kurpas, Jan A1 - Doroshenko, Victor A1 - Suleimanov, Valery F. A1 - Freyberg, Michael A1 - Becker, Werner A1 - Dennerl, Konrad A1 - Haberl, Frank A1 - Lamer, Georg A1 - Maitra, Chandreyee A1 - Potekhin, Alexander Y. A1 - Ramos-Ceja, Miriam E. A1 - Santangelo, Andrea A1 - Traulsen, Iris A1 - Werner, Klaus T1 - Phase-resolved X-ray spectroscopy of PSR B0656+14 with SRG/eROSITA and XMM-Newton JF - Astronomy and astrophysics : an international weekly journal N2 - We present a detailed spectroscopic and timing analysis of X-ray observations of the bright pulsar PSR B0656+14. The observations were obtained simultaneously with eROSITA and XMM-Newton during the calibration and performance verification phase of the Spektrum-Roentgen-Gamma mission (SRG). The analysis of the 100 ks deep observation of eROSITA is supported by archival observations of the source, including XMM-Newton, NuSTAR, and NICER. Using XMM-Newton and NICER, we first established an X-ray ephemeris for the time interval 2015 to 2020, which connects all X-ray observations in this period without cycle count alias and phase shifts. The mean eROSITA spectrum clearly reveals an absorption feature originating from the star at 570 eV with a Gaussian sigma of about 70 eV that was tentatively identified in a previous long XMM-Newton observation. A second previously discussed absorption feature occurs at 260-265 eV and is described here as an absorption edge. It could be of atmospheric or of instrumental origin. These absorption features are superposed on various emission components that are phenomenologically described here as the sum of hot (120 eV) and cold (65 eV) blackbody components, both of photospheric origin, and a power law with photon index Gamma = 2 from the magnetosphere. We created energy-dependent light curves and phase-resolved spectra with a high signal-to-noise ratio. The phase-resolved spectroscopy reveals that the Gaussian absorption line at 570 eV is clearly present throughout similar to 60% of the spin cycle, but it is otherwise undetected. Likewise, its parameters were found to be dependent on phase. The visibility of the line strength coincides in phase with the maximum flux of the hot blackbody. If the line originates from the stellar surface, it nevertheless likely originates from a different location than the hot polar cap. We also present three families of model atmospheres: a magnetized atmosphere, a condensed surface, and a mixed model. They were applied to the mean observed spectrum, whose continuum fit the observed data well. The atmosphere model, however, predicts distances that are too short. For the mixed model, the Gaussian absorption may be interpreted as proton cyclotron absorption in a field as high as 10(14) G, which is significantly higher than the field derived from the moderate observed spin-down. KW - stars: neutron KW - X-rays: stars KW - pulsars: individual: PSR B0656+14 Y1 - 2022 U6 - https://doi.org/10.1051/0004-6361/202141105 SN - 0004-6361 SN - 1432-0746 VL - 661 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Warby, Jonathan A1 - Zu, Fengshuo A1 - Zeiske, Stefan A1 - Gutierrez-Partida, Emilio A1 - Frohloff, Lennart A1 - Kahmann, Simon A1 - Frohna, Kyle A1 - Mosconi, Edoardo A1 - Radicchi, Eros A1 - Lang, Felix A1 - Shah, Sahil A1 - Pena-Camargo, Francisco A1 - Hempel, Hannes A1 - Unold, Thomas A1 - Koch, Norbert A1 - Armin, Ardalan A1 - De Angelis, Filippo A1 - Stranks, Samuel D. A1 - Neher, Dieter A1 - Stolterfoht, Martin T1 - Understanding performance limiting interfacial recombination in pin Perovskite solar cells JF - Advanced energy materials N2 - Perovskite semiconductors are an attractive option to overcome the limitations of established silicon based photovoltaic (PV) technologies due to their exceptional opto-electronic properties and their successful integration into multijunction cells. However, the performance of single- and multijunction cells is largely limited by significant nonradiative recombination at the perovskite/organic electron transport layer junctions. In this work, the cause of interfacial recombination at the perovskite/C-60 interface is revealed via a combination of photoluminescence, photoelectron spectroscopy, and first-principle numerical simulations. It is found that the most significant contribution to the total C-60-induced recombination loss occurs within the first monolayer of C-60, rather than in the bulk of C-60 or at the perovskite surface. The experiments show that the C-60 molecules act as deep trap states when in direct contact with the perovskite. It is further demonstrated that by reducing the surface coverage of C-60, the radiative efficiency of the bare perovskite layer can be retained. The findings of this work pave the way toward overcoming one of the most critical remaining performance losses in perovskite solar cells. KW - C60 KW - defects KW - interface recombination KW - loss mechanisms KW - perovskites KW - solar cells Y1 - 2022 U6 - https://doi.org/10.1002/aenm.202103567 SN - 1614-6832 SN - 1614-6840 VL - 12 IS - 12 PB - Wiley-VCH CY - Weinheim ER - TY - JOUR A1 - Herbst, Konstantin A1 - Baalmann, Lennart R. A1 - Bykov, Andrei A1 - Engelbrecht, N. Eugene A1 - Ferreira, Stefan E. S. A1 - Izmodenov, Vladislav V. A1 - Korolkov, Sergey D. A1 - Levenfish, Ksenia P. A1 - Linsky, Jeffrey L. A1 - Meyer, Dominique M. -A. A1 - Scherer, Klaus A1 - Strauss, R. Du Toit T1 - Astrospheres of planet-hosting cool stars and beyond when modeling meets observations JF - Space science reviews N2 - Thanks to dedicated long-term missions like Voyager and GOES over the past 50 years, much insight has been gained on the activity of our Sun, the solar wind, its interaction with the interstellar medium, and, thus, about the formation, the evolution, and the structure of the heliosphere. Additionally, with the help of multi-wavelength observations by the Hubble Space Telescope, Kepler, and TESS, we not only were able to detect a variety of extrasolar planets and exomoons but also to study the characteristics of their host stars, and thus became aware that other stars drive bow shocks and astrospheres. Although features like, e.g., stellar winds, could not be measured directly, over the past years several techniques have been developed allowing us to indirectly derive properties like stellar mass-loss rates and stellar wind speeds, information that can be used as direct input to existing astrospheric modeling codes. In this review, the astrospheric modeling efforts of various stars will be presented. Starting with the heliosphere as a benchmark of astrospheric studies, investigating the paleo-heliospheric changes and the Balmer H alpha projections to 1 pc, we investigate the surroundings of cool and hot stars, but also of more exotic objects like neutron stars. While pulsar wind nebulae (PWNs) might be a source of high-energy galactic cosmic rays (GCRs), the astrospheric environments of cool and hot stars form a natural shield against GCRs. Their modulation within these astrospheres, and the possible impact of turbulence, are also addressed. This review shows that all of the presented modeling efforts are in excellent agreement with currently available observations. KW - Magneto-hydrodynamic modeling KW - Stochastic differential equations KW - Galactic cosmic rays KW - Heliosphere KW - Astrosphere Y1 - 2022 U6 - https://doi.org/10.1007/s11214-022-00894-3 SN - 0038-6308 SN - 1572-9672 VL - 218 IS - 4 PB - Springer Nature CY - Dordrecht ER - TY - JOUR A1 - Oran, Rona A1 - Weiss, Benjamin P. A1 - Santacruz-Pich, Maria De Soria A1 - Jun, Insoo A1 - Lawrence, David J. A1 - Polanskey, Carol A. A1 - Ratliff, J. Martin A1 - Raymond, Carol A. A1 - Ream, Jodie B. A1 - Russell, Christopher T. A1 - Shprits, Yuri Y. A1 - Zuber, Maria T. A1 - Elkins-Tanton, Linda T. T1 - Maximum energies of trapped particles around magnetized planets and small bodies JF - Geophysical research letters N2 - 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. KW - asteroid magnetospheres KW - (16) Psyche KW - Psyche mission KW - energetic KW - particles KW - chaotic motion KW - hybrid simulations Y1 - 2022 U6 - https://doi.org/10.1029/2021GL097014 SN - 0094-8276 SN - 1944-8007 VL - 49 IS - 13 PB - American Geophysical Union CY - Washington ER - TY - JOUR A1 - Aguilera-Dena, David R. A1 - Langer, Norbert A1 - Antoniadis, John A1 - Pauli, Daniel A1 - Dessart, Luc A1 - Vigna-Gómez, Alejandro A1 - Gräfener, Götz A1 - Yoon, Sung-Chul T1 - Stripped-envelope stars in different metallicity environments: I. Evolutionary phases, classification, and populations JF - Astronomy and astrophysics N2 - 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. KW - stars: massive KW - stars: Wolf-Rayet KW - stars: winds, outflows KW - binaries: general KW - supernovae: general Y1 - 2022 U6 - https://doi.org/10.1051/0004-6361/202142895 SN - 0004-6361 SN - 1432-0746 VL - 661 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Marin-Beloqui, Jose A1 - Zhang, Guanran A1 - Guo, Junjun A1 - Shaikh, Jordan A1 - Wohrer, Thibaut A1 - Hosseini, Seyed Mehrdad A1 - Sun, Bowen A1 - Shipp, James A1 - Auty, Alexander J. A1 - Chekulaev, Dimitri A1 - Ye, Jun A1 - Chin, Yi-Chun A1 - Sullivan, Michael B. A1 - Mozer, Attila J. A1 - Kim, Ji-Seon A1 - Shoaee, Safa A1 - Clarke, Tracey M. T1 - Insight into the origin of trapping in polymer/fullerene blends with a systematic alteration of the fullerene to higher adducts JF - Journal of physical chemistry C N2 - 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. Y1 - 2022 U6 - https://doi.org/10.1021/acs.jpcc.1c10378 SN - 1932-7447 SN - 1932-7455 VL - 126 IS - 5 SP - 2708 EP - 2719 PB - American Chemical Society CY - Washington ER - TY - JOUR A1 - Izotov, Yuri I. A1 - Chisholm, John A1 - Worseck, Gábor A1 - Guseva, Natalia G. A1 - Schaerer, Daniel A1 - Prochaska, Jason Xavier T1 - Lyman alpha and Lyman continuum emission of Mg II-selected star-forming galaxies JF - Monthly notices of the Royal Astronomical Society N2 - We present observations with the Cosmic Origins Spectrograph onboard the Hubble Space Telescope of seven compact low-mass star-forming galaxies at redshifts, z, in the range 0.3161-0.4276, with various O3Mg2 = [O III] lambda 5007/Mg II lambda 2796+2803 and Mg-2 = Mg II lambda 2796/Mg II lambda 2803 emission-line ratios. We aim to study the dependence of leaking Lyman continuum (LyC) emission on the characteristics of Mg ii emission together with the dependencies on other indirect indicators of escaping ionizing radiation. LyC emission with escape fractions f(esc)(LyC) = 3.1-4.6 per cent is detected in four galaxies, whereas only 1 sigma upper limits of f(esc)(LyC) in the remaining three galaxies were derived. A strong narrow Ly alpha emission line with two peaks separated by V-sep similar to 298-592 km s(-1) was observed in four galaxies with detected LyC emission and very weak Ly alpha emission is observed in galaxies with LyC non-detections. Our new data confirm the tight anticorrelation between f(esc)(LyC) and V-sep found for previous low-redshift galaxy samples. V-sep remains the best indirect indicator of LyC leakage among all considered indicators. It is found that escaping LyC emission is detected predominantly in galaxies with Mg-2 greater than or similar to 1.3. A tendency of an increase of f(esc)(LyC) with increasing of both the O3Mg2 and Mg-2 is possibly present. However, there is substantial scatter in these relations not allowing their use for reliable prediction of f(esc)(LyC). KW - galaxies: abundances KW - galaxies: dwarf KW - galaxies: fundamental parameters KW - galaxies: ISM KW - galaxies: starburst KW - dark ages KW - reionization KW - first stars Y1 - 2022 U6 - https://doi.org/10.1093/mnras/stac1899 SN - 0035-8711 SN - 1365-2966 VL - 515 IS - 2 SP - 2864 EP - 2881 PB - Oxford University Press CY - Oxford ER - TY - JOUR A1 - Brinkmann, Kai Oliver A1 - Becker, Tim A1 - Zimmermann, Florian A1 - Kreusel, Cedric A1 - Gahlmann, Tobias A1 - Theisen, Manuel A1 - Haeger, Tobias A1 - Olthof, Selina A1 - Tückmantel, Christian A1 - Günster, M. A1 - Maschwitz, Timo A1 - Göbelsmann, Fabian A1 - Koch, Christine A1 - Hertel, Dirk A1 - Caprioglio, Pietro A1 - Peña-Camargo, Francisco A1 - Perdigón-Toro, Lorena A1 - Al-Ashouri, Amran A1 - Merten, Lena A1 - Hinderhofer, Alexander A1 - Gomell, Leonie A1 - Zhang, Siyuan A1 - Schreiber, Frank A1 - Albrecht, Steve A1 - Meerholz, Klaus A1 - Neher, Dieter A1 - Stolterfoht, Martin A1 - Riedl, Thomas T1 - Perovskite-organic tandem solar cells with indium oxide interconnect JF - Nature N2 - Multijunction solar cells can overcome the fundamental efficiency limits of single-junction devices. The bandgap tunability of metal halide perovskite solar cells renders them attractive for multijunction architectures(1). Combinations with silicon and copper indium gallium selenide (CIGS), as well as all-perovskite tandem cells, have been reported(2-5). Meanwhile, narrow-gap non-fullerene acceptors have unlocked skyrocketing efficiencies for organic solar cells(6,7). Organic and perovskite semiconductors are an attractive combination, sharing similar processing technologies. Currently, perovskite-organic tandems show subpar efficiencies and are limited by the low open-circuit voltage (V-oc) of wide-gap perovskite cells(8) and losses introduced by the interconnect between the subcells(9,10). Here we demonstrate perovskite-organic tandem cells with an efficiency of 24.0 per cent (certified 23.1 per cent) and a high V-oc of 2.15 volts. Optimized charge extraction layers afford perovskite subcells with an outstanding combination of high V-oc and fill factor. The organic subcells provide a high external quantum efficiency in the near-infrared and, in contrast to paradigmatic concerns about limited photostability of non-fullerene cells(11), show an outstanding operational stability if excitons are predominantly generated on the non-fullerene acceptor, which is the case in our tandems. The subcells are connected by an ultrathin (approximately 1.5 nanometres) metal-like indium oxide layer with unprecedented low optical/electrical losses. This work sets a milestone for perovskite-organic tandems, which outperform the best p-i-n perovskite single junctions(12) and are on a par with perovskite-CIGS and all-perovskite multijunctions(13). Y1 - 2022 U6 - https://doi.org/10.1038/s41586-022-04455-0 SN - 0028-0836 SN - 1476-4687 VL - 604 IS - 7905 SP - 280 EP - 286 PB - Nature Research CY - Berlin ER - TY - JOUR A1 - Zapata-Arteaga, Osnat A1 - Marina, Sara A1 - Zuo, Guangzheng A1 - Xu, Kai A1 - Dörling, Bernhard A1 - Alberto Pérez, Luis A1 - Sebastián Reparaz, Juan A1 - Martín, Jaime A1 - Kemerink, Martijn A1 - Campoy-Quiles, Mariano T1 - Design rules for polymer blends with high thermoelectric performance JF - Advanced energy materials N2 - A combinatorial study of the effect of in-mixing of various guests on the thermoelectric properties of the host workhorse polymer poly[2,5-bis(3-tetradecylthiophen-2-yl)thieno[3,2-b]thiophene] (PBTTT) is presented. Specifically, the composition and thickness for doped films of PBTTT blended with different polymers are varied. Some blends at guest weight fractions around 10-15% exhibit up to a fivefold increase in power factor compared to the reference material, leading to zT values around 0.1. Spectroscopic analysis of the charge-transfer species, structural characterization using grazing-incidence wide-angle X-ray scattering, differential scanning calorimetry, Raman, and atomic force microscopy, and Monte Carlo simulations are employed to determine that the key to improved performance is for the guest to promote long-range electrical connectivity and low disorder, together with similar highest occupied molecular orbital levels for both materials in order to ensure electronic connectivity are combined. KW - doping KW - microstructure KW - organic thermoelectrics KW - orientation KW - ternary Y1 - 2022 U6 - https://doi.org/10.1002/aenm.202104076 SN - 1614-6832 SN - 1614-6840 VL - 12 IS - 19 PB - Wiley CY - Weinheim ER - TY - JOUR A1 - Niederhofer, Florian A1 - Cioni, Maria-Rosa L. A1 - Schmidt, Thomas A1 - Bekki, Kenji A1 - de Grijs, Richard A1 - Ivanov, Valentin D. A1 - Oliveira, Joana M. A1 - Ripepi, Vincenzo A1 - Subramanian, Smitha A1 - van Loon, Jacco Th T1 - The VMC survey – XLVI. Stellar proper motions in the centre of the Large Magellanic Cloud JF - Monthly notices of the Royal Astronomical Society N2 - We present proper motion (PM) measurements within the central region of the Large Magellanic Cloud (LMC), using near-infrared data from the VISTA survey of the Magellanic Cloud system (VMC). This work encompasses 18 VMC tiles covering a total sky area of similar to 28 deg(2). We computed absolute stellar PMs from multiepoch observations in the K-s filter over time baselines between similar to 12 and 47 months. Our final catalogue contains similar to 6322 000 likely LMC member stars with derived PMs. We employed a simple flat-rotating disc model to analyse and interpret the PM data. We found a stellar centre of rotation (alpha(0) = 79.95 degrees(+0.22)(-0.23), delta(0) = -69.31 degrees(+0.12)(-0.11)) that is in agreement with that resulting from Hubble Space Telescope data. The inferred viewing angles of the LMC disc (i = 33.5 degrees(+1.2)(-1.3), Theta = 129.8 degrees(+1.9)(-1.9)) are in good agreement with values from the literature but suggest a higher inclination of the central parts of the LMC. Our data confirm a higher rotation amplitude for the young (less than or similar to 0.5 Gyr) stars compared to the intermediate-age/old (greater than or similar to 1 Gyr) population, which can be explained by asymmetric drift. We constructed spatially resolved velocity maps of the intermediate-age/old and young populations. Intermediate-age/old stars follow elongated orbits parallel to the bar's major axis, providing first observational evidence for x(1) orbits within the LMC bar. In the innermost regions, the motions show more chaotic structures. Young stars show motions along a central filamentary bar structure. KW - surveys KW - proper motion KW - stars: kinematics and dynamics KW - galaxies: individual: LMC KW - Magellanic Clouds Y1 - 2022 U6 - https://doi.org/10.1093/mnras/stac712 SN - 0035-8711 SN - 1365-2966 VL - 512 IS - 4 SP - 5423 EP - 5439 PB - Oxford University Press CY - Oxford ER - TY - JOUR A1 - Alvarado-Gómez, Julián D. A1 - Cohen, Ofer A1 - Drake, Jeremy J. A1 - Fraschetti, Federico A1 - Poppenhäger, Katja A1 - Garraffo, Cecilia A1 - Chebly, Judy A1 - Ilin, Ekaterina A1 - Harbach, Laura A1 - Kochukhov, Oleg T1 - Simulating the space weather in the AU Mic system: stellar winds and extreme coronal mass ejections JF - Astrophysical journal N2 - Two close-in planets have been recently found around the M-dwarf flare star AU Microscopii (AU Mic). These Neptune-sized planets (AU Mic b and c) seem to be located very close to the so-called "evaporation valley" in the exoplanet population, making this system an important target for studying atmospheric loss on exoplanets. This process, while mainly driven by high-energy stellar radiation, will be strongly mediated by the space environment surrounding the planets. Here we present an investigation of this last area, performing 3D numerical modeling of the quiescent stellar wind from AU Mic, as well as time-dependent simulations describing the evolution of a highly energetic coronal mass ejection (CME) event in this system. Observational constraints on the stellar magnetic field and properties of the eruption are incorporated in our models. We carry out qualitative and quantitative characterizations of the stellar wind, the emerging CMEs, as well as the expected steady and transient conditions along the orbit of both exoplanets. Our results predict extreme space weather for AU Mic and its planets. This includes sub-Alfvenic regions for the large majority of the exoplanet orbits, very high dynamic and magnetic pressure values in quiescence (varying within 10(2)-10(5) times the dynamic pressure experienced by Earth), and an even harsher environment during the passage of any escaping CME associated with the frequent flaring observed in AU Mic. These space weather conditions alone pose an immense challenge for the survival of exoplanetary atmospheres (if any) in this system. Y1 - 2022 U6 - https://doi.org/10.3847/1538-4357/ac54b8 SN - 1538-4357 VL - 928 IS - 2 PB - IOP Publishing CY - Bristol ER - TY - JOUR A1 - Hovhannisyan, Karen V. A1 - Nemati, Somayyeh A1 - Henkel, Carsten A1 - Anders, Janet T1 - Long-time equilibration can determine transient thermality JF - PRX Quantum N2 - When two initially thermal many-body systems start to interact strongly, their transient states quickly become non-Gibbsian, even if the systems eventually equilibrate. To see beyond this apparent lack of structure during the transient regime, we use a refined notion of thermality, which we call g-local. A system is g-locally thermal if the states of all its small subsystems are marginals of global thermal states. We numerically demonstrate for two harmonic lattices that whenever the total system equilibrates in the long run, each lattice remains g-locally thermal at all times, including the transient regime. This is true even when the lattices have long-range interactions within them. In all cases, we find that the equilibrium is described by the generalized Gibbs ensemble, with three-dimensional lattices requiring special treatment due to their extended set of conserved charges. We compare our findings with the well-known two-temperature model. While its standard form is not valid beyond weak coupling, we show that at strong coupling it can be partially salvaged by adopting the concept of a g-local temperature. Y1 - 2023 U6 - https://doi.org/10.1103/PRXQuantum.4.030321 SN - 2691-3399 VL - 4 IS - 3 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Meyer, Dominique M.-A. A1 - Pohl, Martin A1 - Petrov, M. A1 - Egberts, Kathrin T1 - Mixing of materials in magnetized core-collapse supernova remnants JF - Monthly notices of the Royal Astronomical Society N2 - Core-collapse supernova remnants are structures of the interstellar medium (ISM) left behind the explosive death of most massive stars ( ?40 M-?). Since they result in the expansion of the supernova shock wave into the gaseous environment shaped by the star's wind history, their morphology constitutes an insight into the past evolution of their progenitor star. Particularly, fast-mo ving massiv e stars can produce asymmetric core-collapse superno va remnants. We inv estigate the mixing of materials in core-collapse supernova remnants generated by a moving massive 35 M-? star, in a magnetized ISM. Stellar rotation and the wind magnetic field are time-dependently included into the models which follow the entire evolution of the stellar surroundings from the zero-age main-sequence to 80 kyr after the supernova explosion. It is found that very little main-sequence material is present in remnants from moving stars, that the Wolf-Rayet wind mixes very efficiently within the 10 kyr after the explosion, while the red supergiant material is still unmixed by 30 per cent within 50 kyr after the supernova. Our results indicate that the faster the stellar motion, the more complex the internal organization of the supernova remnant and the more ef fecti ve the mixing of ejecta therein. In contrast, the mixing of stellar wind material is only weakly affected by progenitor motion, if at all. KW - ISM;supernova remnants KW - (magnetohydrodynamics) MHD KW - stars evolution KW - stars: massive Y1 - 2023 U6 - https://doi.org/10.1093/mnras/stad906 SN - 0035-8711 SN - 1365-2966 VL - 521 IS - 4 SP - 5354 EP - 5371 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Mattern, Maximilian A1 - Reppert, Alexander von A1 - Zeuschner, Steffen Peer A1 - Herzog, Marc A1 - Pudell, Jan-Etienne A1 - Bargheer, Matias T1 - Concepts and use cases for picosecond ultrasonics with x-rays JF - Photoacoustics N2 - This review discusses picosecond ultrasonics experiments using ultrashort hard x-ray probe pulses to extract the transient strain response of laser-excited nanoscopic structures from Bragg-peak shifts. This method provides direct, layer-specific, and quantitative information on the picosecond strain response for structures down to few-nm thickness. We model the transient strain using the elastic wave equation and express the driving stress using Gruneisen parameters stating that the laser-induced stress is proportional to energy density changes in the microscopic subsystems of the solid, i.e., electrons, phonons and spins. The laser-driven strain response can thus serve as an ultrafast proxy for local energy-density and temperature changes, but we emphasize the importance of the nanoscale morphology for an accurate interpretation due to the Poisson effect. The presented experimental use cases encompass ultrathin and opaque metal-heterostructures, continuous and granular nanolayers as well as negative thermal expansion materials, that each pose a challenge to established all-optical techniques. KW - Picosecond ultrasonics KW - Ultrafast x-ray diffraction KW - Ultrafast x-ray KW - scattering KW - Ultrafast photoacoustics KW - Nanoscale heat transfer KW - Negative KW - thermal expansion Y1 - 2023 U6 - https://doi.org/10.1016/j.pacs.2023.100503 SN - 2213-5979 VL - 31 PB - Elsevier CY - Amsterdam ER - TY - JOUR A1 - Geist, Emily A1 - Gallagher, John S. A1 - Kotulla, Ralf A1 - Oskinova, Lida A1 - Hamann, Wolf-Rainer A1 - Ramachandran, Varsha A1 - Sabbi, Elena A1 - Smith, Linda J. A1 - Kniazev, Alexey A1 - Nota, Antonella A1 - Rickard, Matthew J. T1 - Ionization and star formation in the giant H ii region SMC-N66 JF - Publications of the Astronomical Society of the Pacific N2 - The NGC 346 young stellar system and associated N66 giant H ii region in the Small Magellanic Cloud are the nearest example of a massive star-forming event in a low metallicity (Z approximate to 0.2Z (circle dot)) galaxy. With an age of less than or similar to 3 Myr this system provides a unique opportunity to study relationships between massive stars and their associated H ii region. Using archival data, we derive a total H alpha luminosity of L(H alpha) = 4.1 x 10(38) erg s(-1) corresponding to an H-photoionization rate of 3 x 10(50) s(-1). A comparison with a predicted stellar ionization rate derived from the more than 50 known O-stars in NGC 346, including massive stars recently classified from Hubble Space Telescope far-ultraviolet (FUV) spectra, indicates an approximate ionization balance. Spectra obtained with SALT suggest the ionization structure of N66 could be consistent with some leakage of ionizing photons. Due to the low metallicity, the FUV luminosity from NGC 346 is not confined to the interstellar cloud associated with N66. Ionization extends through much of the spatial extent of the N66 cloud complex, and most of the cloud mass is not ionized. The stellar mass estimated from nebular L(H alpha) appears to be lower than masses derived from the census of resolved stars which may indicate a disconnect between the formation of high and low mass stars in this region. We briefly discuss implications of the properties of N66 for studies of star formation and stellar feedback in low metallicity environments. Y1 - 2022 U6 - https://doi.org/10.1088/1538-3873/ac697b SN - 0004-6280 SN - 1538-3873 VL - 134 IS - 1036 PB - IOP Publishing CY - Bristol ER - TY - JOUR A1 - Perottoni, Hélio D. A1 - Limberg, Guilherme A1 - Amarante, João A. S. A1 - Rossi, Silvia A1 - Queiroz, Anna B. A. A1 - Santucci, Rafael M. A1 - Pérez-Villegas, Angeles A1 - Chiappini, Cristina T1 - The unmixed debris of Gaia-Sausage/Enceladus in the form of a pair of halo stellar overdensities JF - Astrophysical journal letters N2 - In the first billion years after its formation, the galaxy underwent several mergers with dwarf satellites of various masses. The debris of Gaia-Sausage/Enceladus (GSE), the galaxy responsible for the last significant merger of the Milky Way, dominates the inner halo and has been suggested to be the progenitor of both the Hercules-Aquila Cloud (HAC) and Virgo Overdensity (VOD). We combine SEGUE, APOGEE, Gaia, and StarHorse distances to characterize the chemodynamical properties and verify the link between HAC, VOD, and GSE. We find that the orbital eccentricity distributions of the stellar overdensities and GSE are comparable. We also find that they have similar, strongly peaked, metallicity distribution functions, reinforcing the hypothesis of common origin. Furthermore, we show that HAC and VOD are indistinguishable from the prototypical GSE population within all chemical-abundance spaces analyzed. All these evidences combined provide a clear demonstration that the GSE merger is the main progenitor of the stellar populations found within these halo overdensities. Y1 - 2022 U6 - https://doi.org/10.3847/2041-8213/ac88d6 SN - 2041-8213 VL - 936 IS - 1 PB - IOP Publishing CY - Bristol ER - TY - JOUR A1 - Pranav, Manasi A1 - Hultzsch, Thomas A1 - Musiienko, Artem A1 - Sun, Bowen A1 - Shukla, Atul A1 - Jaiser, Frank A1 - Shoaee, Safa A1 - Neher, Dieter T1 - Anticorrelated photoluminescence and free charge generation proves field-assisted exciton dissociation in low-offset PM6:Y5 organic solar cells JF - APL materials : high impact open access journal in functional materials science N2 - Understanding the origin of inefficient photocurrent generation in organic solar cells with low energy offset remains key to realizing high-performance donor-acceptor systems. Here, we probe the origin of field-dependent free-charge generation and photoluminescence in wnon-fullereneacceptor (NFA)-based organic solar cells using the polymer PM6 and the NFA Y5-a non-halogenated sibling to Y6, with a smaller energetic offset to PM6. By performing time-delayed collection field (TDCF) measurements on a variety of samples with different electron transport layers and active layer thickness, we show that the fill factor and photocurrent are limited by field-dependent free charge generation in the bulk of the blend. We also introduce a new method of TDCF called m-TDCF to prove the absence of artifacts from non-geminate recombination of photogenerated and dark charge carriers near the electrodes. We then correlate free charge generation with steady-state photoluminescence intensity and find perfect anticorrelation between these two properties. Through this, we conclude that photocurrent generation in this low-offset system is entirely controlled by the field-dependent dissociation of local excitons into charge-transfer states. (c) 2023 Author(s). Y1 - 2023 U6 - https://doi.org/10.1063/5.0151580 SN - 2166-532X VL - 11 IS - 6 PB - AIP Publishing CY - Melville ER -