Results 261 to 270 of about 284,450 (301)

Spectroscopic Supermassive Dark Star candidates. [PDF]

Proc Natl Acad Sci U S A
Ilie C, Mahmud SS, Paulin J, Freese K.
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Exploring central star variability of planetary nebulae using gaia photometry. [PDF]

Sci Rep
NegmEldin MA, Ali A, Hamid GM, Essam A.
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Accreting White Dwarfs: An Unreview. [PDF]

Space Sci Rev
Scaringi S, Knigge C, de Martino D.
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Accurate geometric albedo, shape, and size of Hi'iaka from a stellar occultation. [PDF]

Nat Commun
Fernández-Valenzuela E, Ortiz JL, Holler BJ, Sicardy B, Rommel FL, Vara-Lubiano M, Morales N, Vachier F, Desmars J, Kretlow M, Vieira-Martins R, Jehin E, Ferrais M, Santos-Sanz P, Rustamkulov Z, de la Vega A, Warner E, Benkhaldoun Z, Kamin R, Ryan A, Earls B, Conti D, de Wit J, Burdanov A, Francini R, Langill P, Morales R, Fraser W, Kiss C, Pál A, Souami D, Lecacheux J, Braga-Ribas F, Duffard R, Alvarez-Candal A, Benedetti-Rossi G, Morgado B, Camargo JIB, Júnior ARG, Assafin M, Aissa DB, Grigahcene Z, Buie MW, Licandro J, Alarcon MR, Serra-Ricart M, Castro-Tirado A, Fernandez-Garcia EJ, Iglesias-Marzoa R, Galindo-Guil FJ, González H, Gonçalves R, Rengstorf A, Flynn R, Olsen A, Hanna B, Barnes J, A'Hearn JA, Kreyche SM, Miller WJ, Mortensen LE, Gibson TC, Walker G, Stolle-McAllister G, Feiden GA, Froetschel J, Steel S, Encardes D, Fisher RS, Luken A, Holcomb E, Caton D, Dunford B, Monin D.   +73 more
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A Faint Progenitor System for the Faint Supernova 2024vjm

Zimmerman E, Gal-Yam A, Groot P, Ofek E, Roestel Jv, Pastorello A, Valenti S, Ravi A, Chen P, Schulze S, Blagorodnova N, Wavasseur M, Gómez-Muñoz M, Tranin H, de Wet S, Leloudas G, Vreeswijk P, Kwok L, Schwab M, Jha S, Maguire K, Sand D, Stringer E, Kupfer T, Faran T, Anderson J, Andrews J, Andrews M, Badash A, Bloemen S, Bostroem K, Chen T, Valle MD, Dimitriadis G, Dong Y, Farah J, Gillanders J, Godson B, Gromadzki M, Hiramatsu D, Hoang E, Howell D, Janzen D, Kuncarayakti H, Li J, Lyman J, Maeda K, Magee M, Mehta D, Milligan A, Moran S, Ni YQ, O’Neill D, Pearson J, Pieterse D, Pignata G, Reguitti A, Reichart D, Retamal NM, Santos R, Scaringi S, Shrestha M, Srivastav S, Stoppa F, Subrayan B, Valerin G, Wang X, Wynn K, Yaron O, Zang W.   +69 more
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Stellar mass calibration

International Astronomical Union Colloquium, 1978
SummaryAlthough mass results and their evolutionary connotations now largely stem from observational realms other than astrometry, it is the combination with proper motions, kinematics, and distance calibration which significantly enhances their usefulness.
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Stellar mass loss and atmospheric instability

International Astronomical Union Colloquium, 1988
AbstractA review is given of rate of mass-loss values in the upper part of the Hertzsprung-Russell diagram. Near the luminosity limit of stellar existance = −10−4 M⊙ yr−1. Episodical mass loss in bright variable super- and hypergiants does not significantly increase this value. For Wolf-Rayet stars the rate of mass loss is larger by a factor 140 than
Cornelis de Jager, Hans Nieuwenhuijzen
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Stellar Masses and Radii

1989
We have seen that a careful analysis of a star’s spectrum reveals the chemical and physical characteristics of its atmosphere, but the spectrum tells us very little about its deep interior. It gives us only the total amount of radiation emitted per second by the star; it tells us nothing about the generation and transport of this radiation through the ...
Lloyd Motz, Jefferson Hane Weaver
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STELLAR-MASS BLACK HOLES

2014
This chapter examines stellar-mass black holes. The empirical study of black holes began in the 1960s with the discovery of quasars and the advent of X-ray astronomy. X-ray detectors could detect X-rays coming from a particular direction—as the instrument rotated, the detector scanned the sky.
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Stellar mass-luminosity and mass-radius relations

Astrophysics and Space Science, 1991
The new binary star data have been used together with new theoretical estimates in the study of mass-luminosity and mass-radius relations (MLR and MRR) for the Main-Sequence (MS) stars. The slopes of the relations change at certain critical values, e.g., at ∼0.5M⊙ for MLR and at ∼1.7M⊙ for MRR. The first point is the indication of transition from fully-
Osman Demircan, G�ksel Kahraman
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