On total mass loss in stars with masses not exceeding about 8 solar masses

Details On total mass loss in stars with masses not exceeding about 8 solar masses On total mass loss in stars with masses not exceeding about 8 solar masses

Feb 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976a%26a....46..447f&link_type=abstract

Astronomy and Astrophysics, vol. 46, no. 3, Feb. 1976, p. 447-454. Research supported by the Consiglio Nazionale delle Ricerche

Astronomy and Astrophysics

Astrophysics

171

Giant Stars, Stellar Evolution, Stellar Mass Ejection, Supergiant Stars, Supernovae, Astrophysics, Cepheid Variables, Cool Stars, Critical Mass, Hertzsprung-Russell Diagram, Planetary Nebulae, Radiation Pressure

Scientific paper

Two previously obtained mass-loss rates for red giants and supergiants are used to determine the total mass loss experienced by stars with masses not exceeding 8 solar masses and evolving along the first and second red giant branches of the H-R diagram. It is shown that the two rates agree quite closely and give essentially the same results. The masses of white dwarfs are found to depend only to a small extent on the actual value of the mass-loss rate. The dependence of the final mass of a star on a hypothetical mass loss due to an overall instability of the stellar envelope is briefly discussed. The problem of mass loss in cool stars resulting from radiation pressure on dust grains is considered with emphasis on the physical difficulties encountered in attempting to account for the required mass-loss rate. Other astrophysical problems related to mass loss in the red giant phase are briefly examined, including the Cepheid mass discrepancy, the contribution of mass-losing stars to the metal enrichment of the interstellar medium, the origin of planetary nebulae, the structure of pre-supernovae, and the critical mass for carbon detonation.

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