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IRAS and cool stellar mass loss
2008We show that the band strength of the 9.7μm silicate dust feature is well correlated with the CO and OH-maser line strengths, and so provides a reliable measure of mass-loss rates for cool, luminous, Oxygen-rich stars. Correlations are presented between mass-loss rates and various physical properties of the M-Supergiants in the IRAS LRS Catalogue.
C. J. Skinner, B. Whitmore
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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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Stellar Adiabatic Mass Loss in Binary Stars
AIP Conference Proceedings, 2010Stellar adiabatic mass loss model show us the approximate responses of the donor stars suffering rapid mass loss. According to the radius response and the change of total energy during adiabatic mass loss, we present our results on the criteria of dynamical mass transfer instability and the limits on common envelope evolution.
Hongwei Ge +5 more
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Mass Loss in Young Stellar Objects
Astrophysics and Space Science, 1998Various aspects of mass loss associated with Young Stellar Objects are reviewed. The classification of the driving sources of the outflows is presented, and the properties of the youngest sources, the Class 0 protostars, are given. The observed properties of the molecular, atomic, and neutral components of the bipolar flows are discussed and critically
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Mass Loss and Stellar Evolution
1979The available observational evidence about stellar winds and mass loss is briefly reviewed, and its implications for stellar evolution are discussed. Particular emphasis is placed on post-main sequence evolution of low-mass and intermediate-mass stars, including the final evolution from red giant to the white dwarf stage.
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Nucleosynthesis, Mass Loss and Stellar Evolution
1969Stars are formed from material of the interstellar medium with a given composition: X (the fraction of hydrogen), Y (the fraction of helium), Z (the fraction of the sum of the heavy elements, which can be splitted in Z1, Z2, Z3,... representing these heavy elements).
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Stellar mass loss in late B-type supergiants
Astrophysics and Space Science, 1990A study using archive IUE data of time-varying mass loss has been carried out for a sample of 12 supergiants in the spectral range B5–B9. Additionally dedicated IUE velocity-time observations of ‘discrete absorption components’ (DAC) in the UV resonance lines have been made for one of the stars (βOri), while optical data obtained for this star shows ...
S. Gilheany +3 more
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