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The Evolution of Massive Stars with Mass Loss
Annual Review of Astronomy and Astrophysics, 1986Evolution a masse constante. Diagnostic de vents stellaires et parametrisation des taux de perte de masse. Effets de perte de masse sur la structure interne et l'evolution des etoiles massives. Effets de perte de masse sur le diagramme HR d'etoiles lumineuses. Evolution avec depeuplement convectif et perte de masse. Nucleosynthese.
Cesare Chiosi, André Maeder
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Mass Loss from Fast Rotating Stars
1969Evolutionary models of a rotationally unstable 7 M ⊙ star are computed; preliminary results during the H-burning stages are obtained and discussed.
L. NOBILI, SECCO, LUIGI ENRICO
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Mass loss from solar-type stars
Solar Physics, 1985Winds are directly detected from solar-type stars only when they are very young. At ages ~ 106 yr, these stars have mass loss rates ~ 106 times the mass flux of the present solar wind. Although these young T Tauri stars exhibit ultraviolet transition-region and X-ray coronal emission, the large particle densities of the massive winds lead to efficient ...
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Steady mass-loss from supermassive stars
Astrophysics and Space Science, 1986Structures of Newtonian super-massive stars are calculated with the opacity for Compton effect K 0/(1 + αT), where k 0 = 0.2(1 + X) and α = 2.2 × 10−9 K−1. The track of the Main-Sequence is turned right in the upper part of the HR diagram. Mass loss will occur in a Main-Sequence stage for a star with mass larger than a critical mass.
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The asymmetric mass-loss of evolved stars
SPIE Proceedings, 2008The VLTI is a breakthrough for its capabilities to hunt and study asymmetrical circumstillar environments encountered in many targets experiencing large mass-loss rate. These environements provide important information on the perturbations of the wind carrying the mass and momentum lost by the evolved source.
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Weight Loss Strategies and the Risk of Skeletal Muscle Mass Loss
Nutrients, 2021Aloys Berg, David McCarthy
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1980
In Sections 5.5 through 5.8 the theory of expanding spherical stellar atmospheres, and resultant model atmospheres were outlined. This Chapter deals with observations relevant to stellar mass-loss; we describe the way one derives mass-loss values from such observations, summarize and compare M-values, and consider the proposed mechanisms that produce ...
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In Sections 5.5 through 5.8 the theory of expanding spherical stellar atmospheres, and resultant model atmospheres were outlined. This Chapter deals with observations relevant to stellar mass-loss; we describe the way one derives mass-loss values from such observations, summarize and compare M-values, and consider the proposed mechanisms that produce ...
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Mass loss and the Eddington parameter: a new mass-loss recipe for hot and massive stars
Monthly Notices of the Royal Astronomical Society, 2020Joachim Bestenlehner
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Frontal ablation and mass loss of the Patagonian icefields
Earth and Planetary Science Letters, 2021Shin Sugiyama +2 more
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