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EAS Publications Series, 2013
Betelgeuse is just starting to produce a wind which is thick enough to form dust. However, the grains seem to coalesce at much greater distances than those in “dust-driven” winds from later-stage AGB and RSG stars. Is the mass loss mechanism different, and how will it evolve?
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Betelgeuse is just starting to produce a wind which is thick enough to form dust. However, the grains seem to coalesce at much greater distances than those in “dust-driven” winds from later-stage AGB and RSG stars. Is the mass loss mechanism different, and how will it evolve?
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Astrophysics and Space Science, 1979
The evolution of spin in a star undergoing adiabatic mass loss is considered. It is established that adiabatic mass loss cannot drive spin. If such a mass loss is due to a binary component overflowing its Roche lobe then this result rules out the possibility of asynchronous rotation in close contact systems.
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The evolution of spin in a star undergoing adiabatic mass loss is considered. It is established that adiabatic mass loss cannot drive spin. If such a mass loss is due to a binary component overflowing its Roche lobe then this result rules out the possibility of asynchronous rotation in close contact systems.
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1978
The decrease of total mass by ejection past the outer Lagrangian points is a distinct possibility, probably a necessity, in the explanation of late phases of evolution, and some instances have been mentioned earlier. One indication noted by van den Heuvel (1969) may apply to a large fraction of the binary population, namely that much fewer semi ...
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The decrease of total mass by ejection past the outer Lagrangian points is a distinct possibility, probably a necessity, in the explanation of late phases of evolution, and some instances have been mentioned earlier. One indication noted by van den Heuvel (1969) may apply to a large fraction of the binary population, namely that much fewer semi ...
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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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Fragmentation-inactivation models with mass loss
Physical Review E, 1995We consider one-dimensional discrete models for dynamic fragmentation with mass consumption. The fragmentation cascade is randomly interrupted by inactivation of fragments. Exact solutions are obtained. The scaling regimes for the average number of fragments n(s,t) with mass s at time t are investigated for short and long times.
, Machado, , Kamphorst Leal da Silva J
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Science, 2018
Ice Sheets The Greenland Ice Sheet, along with the Antarctic Ice Sheet and glaciers worldwide, is melting at an accelerating rate. This melting is not uniform, however, with adjacent fjords often exhibiting quite different behaviors. What can account for those differences? Millan et al.
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Ice Sheets The Greenland Ice Sheet, along with the Antarctic Ice Sheet and glaciers worldwide, is melting at an accelerating rate. This melting is not uniform, however, with adjacent fjords often exhibiting quite different behaviors. What can account for those differences? Millan et al.
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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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Mira Light Curves and Mass Loss
Astrophysics and Space Science, 1994Long Period Variables represent a late stage in the evolution of intermediate mass stars. Mass loss wich leads them to planetary nebulae within a few 105 years, is a complex process and the object of many investigations. Recents studies suggest that mass loss could occur in brief superwind phases separated by long quiescent periods.
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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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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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