OBSERVATIONS OF DOPPLER BOOSTING IN KEPLER LIGHT CURVES by van Kerkwijk, Marten H., Breton, Rene P., Justham, Stephen, Podsiadlowski, Philipp, Han, Zhanwen, Rappaport, Saul A

“…We re-analyze the Kepler data and demonstrate that both companions are likely to be white dwarfs. We also find that the photometric data for KOI 74 show a modulation in brightness as the more luminous star orbits, due to Doppler boosting. …”
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Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars by Mayusree Das, Banibrata Mukhopadhyay

“…On the other hand, the existence of massive white dwarfs, even violating the Chandrasekhar mass limit, was inferred from the peak luminosities of Type Ia supernovae. …”
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Shock Breakout from Stellar Envelopes: The Relativistic Limit by Tamar Faran, Re'em Sari

“…Finally, we apply our results to explosions in white dwarfs and neutron stars, and find that typical type Ia supernovae emit ∼10 ^41 erg in the form of ∼1 MeV photons.…”
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Data of nearby space objects using SIMBAD astronomical database by Bahram Kalhor

“…The article represents the distance, temperature, and Redshift of 93,060 nearby space objects, including stars, quasars, white dwarfs, and carbon stars. The objects' temperatures are between 671 and 99,575 K, and the distances of the objects are between 413.13 and 0.5 (mas). …”
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The origin of sdB stars (II) by Han, Z, Podsiadlowski, P, Maxted, P, Marsh, T

“…We systematically investigate the importance of the five main evolutionary channels in which the sdB stars form after one or two common-envelope (CE) phases, one or two phases of stable Roche-lobe overflow (RLOF) or as the result of the merger of two helium white dwarfs (WD) (see Han et al. 2002, Paper I). Our best BPS model can satisfactorily explain the main observational characteristics of sdB stars, in particular their distributions in the orbital period - minimum companion mass diagram and in the effective temperature - surface gravity diagram, their distributions of orbital period, log (g theta^4), and mass function, their binary fraction and the fraction of sdB binaries with WD companions, their birthrates and their space density. …”

The Herschel-SPIRE Legacy Survey (HSLS): the scientific goals of a shallow and wide submillimeter imaging survey with SPIRE by Cooray, A, Eales, S, Chapman, S, Clements, D, Dore, O, Farrah, D, Jarvis, M, Kaplinghat, M, Negrello, M, Melchiorri, A, Peiris, H, Pope, A, Santos, MG, Serjeant, S, Thompson, M, White, G, Amblard, A, Banerji, M, Corasaniti, P, Das, S, de_Bernardis, F, de_Zotti, G, Giannantonio, T, Gonzalez, J, Khostovan, A

“…(e) Perform an unbiased survey for star formation and dust at high Galactic latitude and make a census of debris disks and dust around AGB stars and white dwarfs.…”

The CHARA Array Interferometric Program on the Multiplicity of Classical Be Stars: New Detections and Orbits of Stripped Subdwarf Companions by Robert Klement, Thomas Rivinius, Douglas R. Gies, Dietrich Baade, Antoine Mérand, John D. Monnier, Gail H. Schaefer, Cyprien Lanthermann, Narsireddy Anugu, Stefan Kraus, Tyler Gardner

“…The faint, stripped companions can be helium-burning subdwarf OB-type stars (sdOBs), white dwarfs (WDs), or neutron stars. We present optical/near-infrared Center for High Angular Resolution Astronomy (CHARA) interferometry of 37 Be stars selected for spectroscopic indications of low-mass companions. …”
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Hydrodynamic Simulations of Oxygen–Neon Classical Novae as Galactic 7Li Producers and Potential Accretion-induced Collapse Progenitors by Sumner Starrfield, Maitrayee Bose, Christian Iliadis, W. Raphael Hix, Charles E. Woodward, R. Mark Wagner

“…We report on studies of classical nova (CN) explosions where we follow the evolution of thermonuclear runaways (TNRs) on oxygen–neon (ONe) white dwarfs (WDs). Using NOVA, a 1D hydrodynamic computer code, we accrete solar matter until the TNR is ongoing and then switch to a mixed composition. …”
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Search for sub-TeV Neutrino Emission from Novae with IceCube-DeepCore by R. Abbasi, M. Ackermann, J. Adams, N. Aggarwal, J. A. Aguilar, M. Ahlers, J. M. Alameddine, A. A. Alves Jr., N. M. Amin, K. Andeen, T. Anderson, G. Anton, C. Argüelles, Y. Ashida, S. Athanasiadou, S. N. Axani, X. Bai, A. Balagopal V., M. Baricevic, S. W. Barwick, V. Basu, R. Bay, J. J. Beatty, K.-H. Becker, J. Becker Tjus, J. Beise, C. Bellenghi, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, F. Bontempo, J. Y. Book, J. Borowka, C. Boscolo Meneguolo, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, J. Braun, B. Brinson, J. Brostean-Kaiser, R. T. Burley, R. S. Busse, M. A. Campana, E. G. Carnie-Bronca, C. Chen, Z. Chen, D. Chirkin, S. Choi, B. A. Clark, L. Classen, A. Coleman, G. H. Collin, A. Connolly, J. M. Conrad, P. Coppin, P. Correa, S. Countryman, D. F. Cowen, C. Dappen, P. Dave, C. De Clercq, J. J. DeLaunay, D. Delgado López, H. Dembinski, K. Deoskar, A. Desai, P. Desiati, K. D. de Vries, G. de Wasseige, T. DeYoung, A. Diaz, J. C. Díaz-Vélez, M. Dittmer, H. Dujmovic, M. A. DuVernois, T. Ehrhardt, P. Eller, R. Engel, H. Erpenbeck, J. Evans, P. A. Evenson, K. L. Fan, A. R. Fazely, A. Fedynitch, N. Feigl, S. Fiedlschuster, A. T. Fienberg, C. Finley, L. Fischer, D. Fox, A. Franckowiak, E. Friedman, A. Fritz, P. Fürst, T. K. Gaisser, J. Gallagher, E. Ganster, A. Garcia, S. Garrappa, L. Gerhardt, A. Ghadimi, C. Glaser, T. Glauch, T. Glüsenkamp, N. Goehlke, J. G. Gonzalez, S. Goswami, D. Grant, S. J. Gray, T. Grégoire, S. Griffin, S. Griswold, C. Günther, P. Gutjahr, C. Haack, A. Hallgren, R. Halliday, L. Halve, F. Halzen, H. Hamdaoui, M. Ha Minh, K. Hanson, J. Hardin, A. A. Harnisch, P. Hatch, A. Haungs, K. Helbing, J. Hellrung, F. Henningsen, L. Heuermann, S. Hickford, A. Hidvegi, C. Hill, G. C. Hill, K. D. Hoffman, K. Hoshina, W. Hou, T. Huber, K. Hultqvist, M. Hünnefeld, R. Hussain, K. Hymon, S. In, N. Iovine, A. Ishihara, M. Jansson, G. S. Japaridze, M. Jeong, M. Jin, B. J. P. Jones, D. Kang, W. Kang, X. Kang, A. Kappes, D. Kappesser, L. Kardum, T. Karg, M. Karl, A. Karle, U. Katz, M. Kauer, J. L. Kelley, A. Kheirandish, K. Kin, J. Kiryluk, S. R. Klein, A. Kochocki, R. Koirala, H. Kolanoski, T. Kontrimas, L. Köpke, C. Kopper, D. J. Koskinen, P. Koundal, M. Kovacevich, M. Kowalski, T. Kozynets, K. Kruiswijk, E. Krupczak, A. Kumar, E. Kun, N. Kurahashi, N. Lad, C. Lagunas Gualda, M. Lamoureux, M. J. Larson, F. Lauber, J. P. Lazar, J. W. Lee, K. Leonard DeHolton, A. Leszczyńska, M. Lincetto, Q. R. Liu, M. Liubarska, E. Lohfink, C. Love, C. J. Lozano Mariscal, L. Lu, F. Lucarelli, A. Ludwig, W. Luszczak, Y. Lyu, W. Y. Ma, J. Madsen, K. B. M. Mahn, Y. Makino, S. Mancina, W. Marie Sainte, I. C. Mariş, S. Marka, Z. Marka, M. Marsee, I. Martinez-Soler, R. Maruyama, F. Mayhew, T. McElroy, F. McNally, J. V. Mead, K. Meagher, S. Mechbal, A. Medina, M. Meier, S. Meighen-Berger, Y. Merckx, L. Merten, J. Micallef, D. Mockler, T. Montaruli, R. W. Moore, Y. Morii, R. Morse, M. Moulai, T. Mukherjee, R. Naab, R. Nagai, U. Naumann, A. Nayerhoda, J. Necker, M. Neumann, H. Niederhausen, M. U. Nisa, A. Noell, S. C. Nowicki, A. Obertacke Pollmann, M. Oehler, B. Oeyen, A. Olivas, R. Orsoe, J. Osborn, E. O’Sullivan, H. Pandya, D. V. Pankova, N. Park, G. K. Parker, E. N. Paudel, L. Paul, C. Pérez de los Heros, J. Peterson, S. Philippen, S. Pieper, A. Pizzuto, M. Plum, Y. Popovych, M. Prado Rodriguez, B. Pries, R. Procter-Murphy, G. T. Przybylski, C. Raab, J. Rack-Helleis, K. Rawlins, Z. Rechav, A. Rehman, P. Reichherzer, G. Renzi, E. Resconi, S. Reusch, W. Rhode, M. Richman, B. Riedel, E. J. Roberts, S. Robertson, S. Rodan, G. Roellinghoff, M. Rongen, C. Rott, T. Ruhe, L. Ruohan, D. Ryckbosch, D. Rysewyk Cantu, I. Safa, J. Saffer, D. Salazar-Gallegos, P. Sampathkumar, S. E. Sanchez Herrera, A. Sandrock, M. Santander, S. Sarkar, S. Sarkar, J. Savelberg, P. Savina, M. Schaufel, H. Schieler, S. Schindler, B. Schlüter, T. Schmidt, J. Schneider, F. G. Schröder, L. Schumacher, G. Schwefer, S. Sclafani, D. Seckel, S. Seunarine, A. Sharma, S. Shefali, N. Shimizu, M. Silva, B. Skrzypek, B. Smithers, R. Snihur, J. Soedingrekso, A. Søgaard, D. Soldin, C. Spannfellner, G. M. Spiczak, C. Spiering, M. Stamatikos, T. Stanev, R. Stein, T. Stezelberger, T. Stürwald, T. Stuttard, G. W. Sullivan, I. Taboada, S. Ter-Antonyan, W. G. Thompson, J. Thwaites, S. Tilav, K. Tollefson, C. Tönnis, S. Toscano, D. Tosi, A. Trettin, C. F. Tung, R. Turcotte, J. P. Twagirayezu, B. Ty, M. A. Unland Elorrieta, K. Upshaw, N. Valtonen-Mattila, J. Vandenbroucke, N. van Eijndhoven, D. Vannerom, J. van Santen, J. Vara, J. Veitch-Michaelis, S. Verpoest, D. Veske, C. Walck, T. B. Watson, C. Weaver, P. Weigel, A. Weindl, J. Weldert, C. Wendt, J. Werthebach, M. Weyrauch, N. Whitehorn, C. H. Wiebusch, N. Willey, D. R. Williams, M. Wolf, G. Wrede, J. Wulff, X. W. Xu, J. P. Yanez, E. Yildizci, S. Yoshida, S. Yu, T. Yuan, Z. Zhang, P. Zhelnin, IceCube Collaboration

“…The understanding of novae, the thermonuclear eruptions on the surfaces of white dwarf stars in binaries, has recently undergone a major paradigm shift. …”
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Tracing the Evolution of SMBHs and Stellar Objects in Galaxy Mergers: A Multi-mass Direct N-body Model by Shuo Li, Shiyan Zhong, Peter Berczik, Rainer Spurzem, Xian Chen, F. K. Liu

“…Special schemes have also been developed to deal with some rare but interesting events, such as the tidal disruption of main-sequence stars, plunging low-mass stars, white dwarfs, neutron stars and stellar-mass black holes, and the partial tidal disruption of red giants or asymptotic giant branch stars. …”
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Iron-rich Metal-poor Stars and the Astrophysics of Thermonuclear Events Observationally Classified as Type Ia Supernovae. I. Establishing the Connection by Henrique Reggiani, Kevin C. Schlaufman, Andrew R. Casey

“…We find that the elemental abundances of BD +80 245, HE 0533–5340, and SMSS J034249.53–284216.0 are best explained by the (double) detonations of sub-Chandrasekhar-mass CO white dwarfs. If our interpretation of IRMP stars is accurate, then they should be very rare in globular clusters and more common in the Magellanic Clouds and dwarf spheroidal galaxies than in the Milky Way’s halo. …”
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Origin and Composition of the Galactic Diffuse X-Ray Emission Spectra by Unresolved X-Ray Sources by Katsuji Koyama, Masayoshi Nobukawa

“…The X-ray spectra of GDXE are expressed by the assembly of compact X-ray sources, which are either white dwarfs (WDs) or X-ray active stars consisting of binaries with late-type stars. …”
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The wide-field, multiplexed, spectroscopic facility WEAVE: survey design, overview, and simulated implementation by Jin, S, Trager, S, Dalton, GB, Aguerri, JAL, Drew, J, Falcón-Barroso, J, Gänsicke, B, Hill, V, Iovino, A, Pieri, M, Poggianti, B, Smith, D, Vallenari, A, Abrams, DC, Aguado, D, Ascasibar, Y, Belokurov, V, Laigle, C, Molaeinezhad, A, Terrett, D, Gilbert, J, Hughes, S, Jarvis, M, Lewis, I, Peirani, S, Schallig, E, Stott, J

“…After summarising the design and implementation of WEAVE and its data systems, we present the organisation, science drivers and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy’s origins by completing Gaia’s phase-space information, providing metallicities to its limiting magnitude for ∼3 million stars and detailed abundances for ∼1.5 million brighter field and open-cluster stars; (ii) survey ∼0.4 million Galactic-plane OBA stars, young stellar objects and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey ∼400 neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionised gas in z < 0.5 cluster galaxies; (vi) survey stellar populations and kinematics in ∼25 000 field galaxies at 0.3 ≲ z ≲ 0.7; (vii) study the cosmic evolution of accretion and star formation using >1 million spectra of LOFAR-selected radio sources; (viii) trace structures using intergalactic/circumgalactic gas at z > 2. …”

The effects of binary evolution on the dynamics of core collapse and neutron star kicks by Podsiadlowski, P, Langer, N, Poelarends, A, Rappaport, S, Heger, A, Pfahl, E

“…We find that the initially more massive stars in binary systems with masses in the range 8-11 M ⊙ are likely to undergo an electron-capture supernova, while single stars in the same mass range would end as ONeMg white dwarfs. We suggest that the core collapse k an electron-capture supernova (and possibly in the case of relatively small iron cores) leads to a prompt or fast explosion rather than a very slow, delayed neutrino-driven explosion and that this naturally produces neutron stars with low-velocity kicks. …”

The origin of subdwarf B star - I: The formation channels by Han, Z, Podsiadlowski, P, Maxted, P, Marsh, T, Ivanova, N

“…To understand their formation better, we present the results of a detailed investigation of the three main binary evolution channels that can lead to the formation of sdB stars: the common-envelope (CE) ejection channel, the stable Roche lobe overflow (RLOF) channel, and the double helium white dwarfs (WDs) merger channel. The CE ejection channel leads to the formation of sdB stars in short-period binaries with typical orbital periods between 0.1 and 10 d, very thin hydrogen-rich envelopes and a mass distribution sharply peaked around ∼0.46 M⊙. …”

The effects of binary evolution on the dynamics of core collapse and neutron-star kicks by Podsiadlowski, P, Langer, N, Poelarends, A, Rappaport, S, Heger, A, Pfahl, E

“…We find that the initially more massive stars in binary systems with masses in the range 8-11 M☉ are likely to undergo an electron-capture supernova, while single stars in the same mass range would end as ONeMg white dwarfs. We suggest that the core collapse in an electron-capture supernova (and possibly in the case of relatively small iron cores) leads to a prompt or fast explosion rather than a very slow, delayed neutrino-driven explosion and that this naturally produces neutron stars with low-velocity kicks. …”

Modeling the Chemical Enrichment History of the Bulge Fossil Fragment Terzan 5 by Donatella Romano, Francesco R. Ferraro, Livia Origlia, Simon Portegies Zwart, Barbara Lanzoni, Chiara Crociati, Davide Massari, Emanuele Dalessandro, Alessio Mucciarelli, R. Michael Rich, Francesco Calura, Francesca Matteucci

“…The iron content of the youngest stellar population is better explained if the white dwarfs that give rise to type Ia supernovae (the main Fe factories) sink toward the cluster center, rather than being stripped by the strong tidal forces exerted by the Milky Way in the outer regions.…”
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Revisiting the Oldest Stars as Cosmological Probes: New Constraints on the Hubble Constant by Andrea Cimatti, Michele Moresco

“…To this purpose, we selected from the literature the oldest objects (globular clusters, stars, white dwarfs, and ultrafaint and dwarf spheroidal galaxies) with accurate age estimates. …”
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Absolute Calibration. III. Improved Absolute Calibration for the Visible through the Mid-infrared by G. H. Rieke, Charles Engelke, Kate Su, Luca Casagrande

“…G-stars older than ∼1 Gyr are good candidates if accurate temperatures can be measured. White dwarfs are suitable from the visible through the near-infrared, but their properties are unexplored at the necessary level at the longer infrared wavelengths, and for most facilities they are too faint there. …”
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A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra by Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra

“…We further improve the model by extending it to brown dwarfs, as well as white dwarfs, resulting in a comprehensive coverage between 1700 < T _eff < 100,000 K and 0 < $\mathrm{log}g$ < 10, to ensure BOSS Net can reliably measure parameters of most of the commonly observed objects within this parameter space. …”
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