The most massive stars in the Galaxy and the LMC - Quasi-homogeneous evolution, time-averaged mass loss rates and mass limits

Details The most massive stars in the Galaxy and the LMC - Quasi-homogeneous evolution, time-averaged mass loss rates and mass limits The most massive stars in the Galaxy and the LMC - Quasi-homogeneous evolution, time-averaged mass loss rates and mass limits

Dec 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....92..101m&link_type=abstract

Astronomy and Astrophysics, vol. 92, no. 1-2, Dec. 1980, p. 101-110.

Astronomy and Astrophysics

Astrophysics

106

Magellanic Clouds, Milky Way Galaxy, Stellar Evolution, Stellar Mass, Supermassive Stars, Hertzsprung-Russell Diagram, O Stars, Stellar Envelopes, Stellar Mass Ejection, Stellar Models

Scientific paper

Numerical models are used to study the evolution of massive stars in the range 15-240 solar masses with two chemical compositions appropriate for the Galaxy and the LMC and various mass loss rates. It is found that stars with mass not less than 100 solar masses and time-averaged mass loss rates not less than 0.00002 solar mass/yr evolve, after a stay near the main sequence, directly toward the left in the HR diagram. Their interiors progressively tend, during the H-burning phase, toward a quasi-homogeneous structure as a result of mass loss: the large homogeneous core is surrounded by an envelope showing very little composition difference between the core surface and the stellar surface. The time-averaged mass loss rates of the most massive stars in the Galaxy and LMC are estimated on the basis of the upper limit of the distribution of O stars in the HR diagrams by Humphreys (1978, 1979) and Humphreys and Davidson (1979).

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