Results 1 to 10 of about 15,296 (313)
PEPSI Investigation, Retrieval, and Atlas of Numerous Giant Atmospheres (PIRANGA). IV. High-resolution Phased-resolved Spectroscopy of the Ultra-hot-Jupiter KELT-20 b. [PDF]
Astron JBonidie V +9 more
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Tidal tail identification and detailed analysis of the open star cluster King 13 using Gaia DR3 and 2MASS. [PDF]
Sci RepAhmed NM, Darwish MS.
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Estimation of mass and radii for charged compact objects using a modified Chaplygin equation of state in the Buchdahl-I metric. [PDF]
PLoS OneZahra A +4 more
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The Progenitor Systems of Classical Novae in M31. [PDF]
Astrophys JAbelson CS +6 more
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Acoustic modes in M67 cluster stars trace deepening convective envelopes. [PDF]
NatureReyes C +5 more
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Eclipsing Binary Systems as Tests of Low-Mass Stellar Evolution Theory
, 2015 Gregory A. Feiden
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Some of the next articles are maybe not open access.
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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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, 1988AbstractA 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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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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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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