SN 2016ije: An SN 2002es-like Type Ia Supernova Exploded in a Metal-poor and Low-surface Brightness Galaxy by Zhitong Li, Tianmeng Zhang, Xiaofeng Wang, Jujia Zhang, Lluís Galbany, Alexei V. Filippenko, Thomas G. Brink, Chris Ashall, WeiKang Zheng, Thomas de Jaeger, Fabio Ragosta, Maxime Deckers, Mariusz Gromadzki, D. R. Young, Gaobo Xi, Juncheng Chen, Xulin Zhao, Hanna Sai, Shengyu Yan, Danfeng Xiang, Zhihao Chen, Wenxiong Li, Bo Wang, Hu Zou, Jipeng Sui, Jiali Wang, Jun Ma, Jundan Nie, Suijian Xue, Xu Zhou, Zhimin Zhou

“…These characteristics suggest that SN 2016ije might originate from the violent merger of a white dwarf binary system, when viewed near an orientation along the iron-group-element cavity caused by the companion star.…”
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OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting Either a Late-type Star or a Stellar Remnant by Rintaro Kirikawa, Takahiro Sumi, David P. Bennett, Daisuke Suzuki, Naoki Koshimoto, Shota Miyazaki, Ian A. Bond, Andrzej Udalski, Nicholas J. Rattenbury, Leading Authors, Fumio Abe, Richard Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Yutaka Matsubara, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki K. Satoh, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita, MOA COLLABORATION, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Mateusz J. Mróz, OGLE COLLABORATION

“…Bayesian inference is used to estimate the physical parameters of the lens, revealing that the shorter timescale model predicts 65% and 25% probabilities of a late-type star and white dwarf host, respectively, while the longer timescale model favors a black hole host with a probability ranging from 60% to 95%, under the assumption that stars and stellar remnants have equal probabilities of hosting companions with planetary mass ratios. …”
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Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility by Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao

“…They could evolve to form white dwarfs or explode as electron-capture supernovae (SNe) or iron core-collapse SNe (CCSNe). …”
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Asteroseismology and Spectropolarimetry of the Exoplanet Host Star λ Serpentis by Travis S. Metcalfe, Derek Buzasi, Daniel Huber, Marc H. Pinsonneault, Jennifer L. van Saders, Thomas R. Ayres, Sarbani Basu, Jeremy J. Drake, Ricky Egeland, Oleg Kochukhov, Pascal Petit, Steven H. Saar, Victor See, Keivan G. Stassun, Yaguang Li, Timothy R. Bedding, Sylvain N. Breton, Adam J. Finley, Rafael A. García, Hans Kjeldsen, Martin B. Nielsen, J. M. Joel Ong, Jakob L. Rørsted, Amalie Stokholm, Mark L. Winther, Catherine A. Clark, Diego Godoy-Rivera, Ilya V. Ilyin, Klaus G. Strassmeier, Sandra V. Jeffers, Stephen C. Marsden, Aline A. Vidotto, Sallie Baliunas, Willie Soon

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SN 2022joj: A Potential Double Detonation with a Thin Helium Shell by E. Padilla Gonzalez, D. A. Howell, G. Terreran, C. McCully, M. Newsome, J. Burke, J. Farah, C. Pellegrino, K. A. Bostroem, G. Hosseinzadeh, J. Pearson, D. J. Sand, M. Shrestha, N. Smith, Y. Dong, N. Meza Retamal, S. Valenti, S. Boos, K. J. Shen, D. Townsley, L. Galbany, L. Piscarreta, R. J. Foley, M. J. Bustamante-Rosell, D. A. Coulter, R. Chornock, K. W. Davis, C. B. Dickinson, D. O. Jones, J. Kutcka, X. K. Le Saux, C. R. Rojas-Bravo, K. Taggart, S. Tinyanont, G. Yang, S. W. Jha, R. Margutti

“…Spectroscopically, we find strong agreement between SN 2022joj and double detonation models with white dwarf masses of around 1 M _⊙ and a thin He shell between 0.01 and 0.05 M _⊙ . …”
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JWST Low-resolution MIRI Spectral Observations of SN 2021aefx: High-density Burning in a Type Ia Supernova by J. M. DerKacy, C. Ashall, P. Hoeflich, E. Baron, B. J. Shappee, D. Baade, J. Andrews, K. A. Bostroem, P. J. Brown, C. R. Burns, A. Burrow, A. Cikota, T. de Jaeger, A. Do, Y. Dong, I. Dominguez, L. Galbany, E. Y. Hsiao, E. Karamehmetoglu, K. Krisciunas, S. Kumar, J. Lu, T. B. Mera Evans, J. R. Maund, P. Mazzali, K. Medler, N. Morrell, F. Patat, M. M. Phillips, M. Shahbandeh, S. Stangl, C. P. Stevens, M. D. Stritzinger, N. B. Suntzeff, C. M. Telesco, M. A. Tucker, S. Valenti, L. Wang, Y. Yang, S. W. Jha, L. A. Kwok

“…Emission line profiles and the presence of electron capture elements are used to constrain the mass of the exploding white dwarf (WD) and the chemical asymmetries in the ejecta. …”
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TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems by Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab

“…TOI-3984 A ( J = 11.93) is an M4 dwarf hosting a short-period (4.353326 ± 0.000005 days) gas giant ( M _p = 0.14 ± 0.03 M _J and R _p = 0.71 ± 0.02 R _J ) with a wide-separation white dwarf companion. TOI-5293 A ( J = 12.47) is an M3 dwarf hosting a short-period (2.930289 ± 0.000004 days) gas giant ( M _p = 0.54 ± 0.07 M _J and R _p = 1.06 ± 0.04 R _J ) with a wide-separation M dwarf companion. …”
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PSR J2150+3427: A Possible Double Neutron Star System by Q. D. Wu, N. Wang, J. P. Yuan, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, S. Q. Wang, S. N. Sun, F. F. Kou, D. Zhao, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang

“…An estimate for the total mass of the system using the $\dot{\omega }$ gives M _tot = 2.59(13) M _⊙ , which is consistent with most of the known double neutron star (DNS) systems and one neutron star (NS)–white dwarf (WD) system named B2303+46. Combining $\dot{\omega }$ with the mass function of the system gives the masses of M _p < 1.67 and M _c > 0.98 M _⊙ for the pulsar and the companion star, respectively. …”
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The Initial Mass Function Based on the Full-sky 20 pc Census of ∼3600 Stars and Brown Dwarfs by J. Davy Kirkpatrick, Federico Marocco, Christopher R. Gelino, Yadukrishna Raghu, Jacqueline K. Faherty, Daniella C. Bardalez Gagliuffi, Steven D. Schurr, Kevin Apps, Adam C. Schneider, Aaron M. Meisner, Marc J. Kuchner, Dan Caselden, R. L. Smart, S. L. Casewell, Roberto Raddi, Aurora Kesseli, Nikolaj Stevnbak Andersen, Edoardo Antonini, Paul Beaulieu, Thomas P. Bickle, Martin Bilsing, Raymond Chieng, Guillaume Colin, Sam Deen, Alexandru Dereveanco, Katharina Doll, Hugo A. Durantini Luca, Anya Frazer, Jean Marc Gantier, Léopold Gramaize, Kristin Grant, Leslie K. Hamlet, Hiro Higashimura, Michiharu Hyogo, Peter A. Jałowiczor, Alexander Jonkeren, Martin Kabatnik, Frank Kiwy, David W. Martin, Marianne N. Michaels, William Pendrill, Celso Pessanha Machado, Benjamin Pumphrey, Austin Rothermich, Rebekah Russwurm, Arttu Sainio, John Sanchez, Fyodor Theo Sapelkin-Tambling, Jörg Schümann, Karl Selg-Mann, Harshdeep Singh, Andres Stenner, Guoyou Sun, Christopher Tanner, Melina Thévenot, Maurizio Ventura, Nikita V. Voloshin, Jim Walla, Zbigniew Wędracki, Jose I. Adorno, Christian Aganze, Katelyn N. Allers, Hunter Brooks, Adam J. Burgasser, Emily Calamari, Thomas Connor, Edgardo Costa, Peter R. Eisenhardt, Jonathan Gagné, Roman Gerasimov, Eileen C. Gonzales, Chih-Chun Hsu, Rocio Kiman, Guodong Li, Ryan Low, Eric Mamajek, Blake M. Pantoja, Mark Popinchalk, Jon M. Rees, Daniel Stern, Genaro Suárez, Christopher Theissen, Chao-Wei Tsai, Johanna M. Vos, David Zurek, (The Backyard Worlds: Planet 9 Collaboration)

“…A complete accounting of nearby objects—from the highest-mass white dwarf progenitors down to low-mass brown dwarfs—is now possible, thanks to an almost complete set of trigonometric parallax determinations from Gaia, ground-based surveys, and Spitzer follow-up. …”
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Hunting for the progenitor of SN 1006: High resolution spectroscopic search with the FLAMES instrument by Kerzendorf, W, Schmidt, B, Laird, J, Podsiadlowski, P, Bessell, MS

“…It is widely believed that these events are the thermonuclear explosions of carbon-oxygen white dwarfs close to the Chandrasekhar mass (1.38 M\odot). …”

Semi-analytical formulas for the Hertzsprung-Russell diagram by Zaninetti L.

“…This new technique is applied to the first 10 pc, the first 50 pc, the Hyades and to the determination of the distance of a cluster. The case of the white dwarfs is analyzed assuming the absence of calibrated data: our equation produces a smaller χ2 with respect to the standard color-magnitude calibration when applied to the Villanova Catalog of Spectroscopically Identified White Dwarfs. …”
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Preface of “Asymmetric Planetary Nebulae 8e” by Martin A. Guerrero, Quentin A. Parker, Noam Soker

“…Planetary nebulae (PNe) are the progeny of low- and intermediate-mass stars, at the exact time in their late evolution when they eject their hydrogen-rich envelopes and start their transition towards white dwarfs [...]…”
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Stellar cooling limits on light scalar boson revisited by Yasuhiro Yamamoto, Koichi Yoshioka

“…We obtain limits on the Higgs-scalar mixing angle of 10−10–10−9, which are given by white dwarfs or red giants up to the luminosity limits, in the region where the scalar mass is lighter than about 10 keV.…”
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A two-stream formalism for the convective Urca process by Lesaffre, P, Podsiadlowski, P, Tout, C

“…We conclude that the proper modelling of the Urca process is essential for determining the ignition conditions for the thermonuclear runaway in Chandrasekhar-mass white dwarfs.…”

Analysis of the fractional relativistic polytropic gas sphere by Mohamed S. Aboueisha, Mohamed I. Nouh, Emad A. -B. Abdel-Salam, Tarek M. Kamel, M. M. Beheary, Kamel A. K. Gadallah

“…Abstract Many stellar configurations, including white dwarfs, neutron stars, black holes, supermassive stars, and star clusters, rely on relativistic effects. …”
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The formation of hydrogen-deficient stars in binaries by Podsiadlowski, P

“…Here I review the main binary interactions, stable and unstable mass transfer, binary mergers, and apply them to a variety of objects. including hot subdwarfs, He-rich sdO stars, AM CVn stars, Type Ia supernova progenitors, ultracool white dwarfs and Type Ic and gamma-ray burst progenitors.…”

Galactic Model Parameters and Spatial Density of Cataclysmic Variables in the Gaia Era: New Constraints on Population Models by Remziye Canbay, Selçuk Bilir, Aykut Özdönmez, Tansel Ak

“…A comparison of the luminosity function of white dwarfs with the luminosity function of all CVs in this study show that 500 times the luminosity function of CVs fits very well to the luminosity function of white dwarfs. …”
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The progenitors of sdB binaries: Confronting theory with observations by Podsiadlowski, P, Han, Z

“…We have re-examined the main binary evolution channels that produce sdB stars ( by stable and unstable mass transfer, the merging of two helium white dwarfs). We find that all three main channels are of comparable importance, but produce slightly different mass distributions and dominate at different times. …”

Concluding remarks by Stone, N

“…It is particularly important to study the evolutionary links between white dwarfs and subdwarf-B stars with stars considered to have been their progenitors, those on the Red Giant and Asymptotic Giant Branches. …”

Supersoft X-ray sources as transient phases of cataclysmic variable evolution by Webbink, R

“…Such systems are concentrated in orbital period just above the period gap, and can, in the most favorable circumstances, achieve X-ray lifetimes in excess of 3 x 10(5) yr. They have white dwarfs of moderate mass (0.7 - 0.9 M.), and may therefore tend to lower X-ray temperatures and luminosities than the more populous, longer-period supersoft sources with donor masses exceeding similar to 1.5 M.. …”