Very massive stars - Evolution with mass loss. I - The hydrogen and helium burning phase

Details Very massive stars - Evolution with mass loss. I - The hydrogen and helium burning phase Very massive stars - Evolution with mass loss. I - The hydrogen and helium burning phase

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..93..313k&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 93, no. 2, June 1983, p. 313-345. Research supported by the Consejo Nacion

Astronomy and Astrophysics

Astrophysics

21

Abundance, Hertzsprung-Russell Diagram, Nuclear Reactions, Stellar Evolution, Stellar Mass Ejection, Supermassive Stars, Convective Flow, Early Stars, Helium, Hydrogen, Mass To Light Ratios, Molecular Weight, Stellar Structure, Stellar Temperature

Scientific paper

The evolution of mass-losing very massive stars in the 500-10000 M_sun; range has been investigated for two different initial compositions, (X,Z) = (0.8,0.0) and (X,Z) = (1.0,0.0). The evolutionary tracks are governed by two opposing factors which are the increase in the mean molecular weight in the convective core and the effect of mass loss. Conservative evolution of stars with masses M very low 10000 M_sun; is similar to that of massive stars (20-100 M_sun;), always moving to lower effective temperatures. For low values of the standard mass loss parameter N (50 ⪉ N ⪉ 200) the two opposing factors are almost in balance and the star is forced to move in a series of loops. For higher mass loss rates the loops disappear. In the 10000 M_sun; case no loops are observed and the tracks always move to higher effective temperatures. For a given mass loss rate the transition between right and left moving tracks occurs at higher masses the lower is the mass loss rate.

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