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The Wolf-Rayet stars and mass loss
Astrophysics and Space Science, 1969Wolf-Rayet stars are defined, a summary is given of the properties of Wolf-Rayet stars, and a qualitative model of a Wolf-Rayet star is sketched. It is incontrovertible that Wolf-Rayet stars are losing mass, a typical rate of mass loss being near 10-5 M ⊙ per year.
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Rotational mass loss by Be stars
Astronomy Reports, 2003We have carried out a numerical study of rotational mass loss by rapidly rotating Be stars assuming preservation of rigid-body rotation during their main-sequence evolution. Evolutionary models are computed for stars with solar chemical composition and initial masses of 3, 10 and M⊙. As a result of their rapid initial rotation, these stars can lose one
A. V. Tutukov, A. V. Fedorova
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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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Symposium - International Astronomical Union, 1970
In this summary we shall attempt to evaluate the mass loss from several kinds of high luminosity stars, especially planetary nebulae, OB supergiants and M giants and supergiants. The purpose is to give an observational basis for the discussion of the mechanism of mass loss and of the consequences of stellar mass loss for the interstellar medium and for
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In this summary we shall attempt to evaluate the mass loss from several kinds of high luminosity stars, especially planetary nebulae, OB supergiants and M giants and supergiants. The purpose is to give an observational basis for the discussion of the mechanism of mass loss and of the consequences of stellar mass loss for the interstellar medium and for
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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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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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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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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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Evidence for mass loss in visual binary stars
Astrophysics and Space Science, 1988The present status of the observational evidence about mass loss in visual binary and multiple systems is reviewed. Particular emphasis is placed on the importance of mass-loss rates measures in these stars, as a systematic study would provide useful constraints in two fields. First, as mass-outflows processes are not modified by the interaction of the
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