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Publications of the Astronomical Society of Australia, 1977
The visual spectra of some hot stars, including P Cygni, have emission with associated absorption troughs ˜ 102 km s-1 on the short-wavelength side (Beals 1929, 1951). These P Cygni profiles are easily understood in terms of mass flowing away from the star.
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The visual spectra of some hot stars, including P Cygni, have emission with associated absorption troughs ˜ 102 km s-1 on the short-wavelength side (Beals 1929, 1951). These P Cygni profiles are easily understood in terms of mass flowing away from the star.
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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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2001
Stars return mass to the interstellar medium throughout their lives. A low-luminosity star such as the Sun is losing mass by a stellar wind at a rate of 10-14 solar masses per year (M ⊙yr-1). Very luminous stars, whether they are early-type hot stars or cool giants, lose mass at a rate of up to about 10-5 M ⊙yr- 1, and such rates have major ...
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Stars return mass to the interstellar medium throughout their lives. A low-luminosity star such as the Sun is losing mass by a stellar wind at a rate of 10-14 solar masses per year (M ⊙yr-1). Very luminous stars, whether they are early-type hot stars or cool giants, lose mass at a rate of up to about 10-5 M ⊙yr- 1, and such rates have major ...
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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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Publications of the Astronomical Society of the Pacific, 1988
This work consists of two studies of the matter that flows outward from the surface of stars that have reached the late stages of evolution. This process of mass loss is important to the understanding of the continued evolution of the star and the replenishment of the interstellar medium from which the next generation of stars will form.
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This work consists of two studies of the matter that flows outward from the surface of stars that have reached the late stages of evolution. This process of mass loss is important to the understanding of the continued evolution of the star and the replenishment of the interstellar medium from which the next generation of stars will form.
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1997
The phase of high mass loss, one of the ultimate phases of stellar evolution, is still poorly known. For a long time, large visual extinctions and small angular sizes have impeded the study of the most interesting objects in this stage. The recent development of mm and IR interferometry has allowed a breakthrough in this domain.
M. Guélin, R. Lucas, R. Neri
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The phase of high mass loss, one of the ultimate phases of stellar evolution, is still poorly known. For a long time, large visual extinctions and small angular sizes have impeded the study of the most interesting objects in this stage. The recent development of mm and IR interferometry has allowed a breakthrough in this domain.
M. Guélin, R. Lucas, R. Neri
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1982
A general overview is drawn concerning the present day status on the problem of mass loss from stars. After an introductory part summarizing its classical interpretations, a general comparison is sketched between mass conserving and mass losing evolutions for supergiant stars, for which mass loss effects are expected to have the largest importance; and
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A general overview is drawn concerning the present day status on the problem of mass loss from stars. After an introductory part summarizing its classical interpretations, a general comparison is sketched between mass conserving and mass losing evolutions for supergiant stars, for which mass loss effects are expected to have the largest importance; and
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1986
Mass loss by cool giant stars is very likely the most important mechanism for returning processed stellar material to the interstellar medium. This mass loss has profound effects on the evolution of individual intermediate mass stars and the chemical evolution of the Milky Way. The IRAS point source catalog is ideally suited for identifying those stars
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Mass loss by cool giant stars is very likely the most important mechanism for returning processed stellar material to the interstellar medium. This mass loss has profound effects on the evolution of individual intermediate mass stars and the chemical evolution of the Milky Way. The IRAS point source catalog is ideally suited for identifying those stars
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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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