Effects of accretion onto massive main sequence stars.

Details Effects of accretion onto massive main sequence stars. Effects of accretion onto massive main sequence stars.

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...297..483b&link_type=abstract

Astronomy and Astrophysics, v.297, p.483

Astronomy and Astrophysics

Astrophysics

57

Stars: Early-Type, Stars: Evolution, Stars: Binaries: Close, Convection, Accretion

Scientific paper

We investigate the effect of mass accretion onto massive main sequence stars on their internal structure and evolution. Adopted accretion rates and accretion time scales are in the range applying to massive Case B binary systems. For the first time, we incorporate the influence of molecular weight gradients on convection in this context. In contrast to earlier studies, we find that the so called "rejuvenation" of the mass accreting star does not always take place. Rather, stellar models with a chemical structure unlike that of single stars may be obtained. We investigate which physical parameters determine whether rejuvenation occurs, namely the fraction of the core hydrogen burning time spent until the onset of accretion, the amount of matter accreted, the initial mass of the accreting star, and the efficiency of convection in regions of stabilizing mean molecular weight gradients. Further on, the evolution of accretion stars until central carbon ignition is investigated. We find that the main result of non-rejuvenation is a much smaller helium core mass and accordingly longer core helium burning times compared to single stars. This may lead to blue supergiant positions adjacent to the main sequence band in the HR diagram, and to blue supergiant pre-supernova configurations. Possible relations to the observed distribution of luminous stars in the HR diagram of the LMC and to the progenitor of supernova 1987A are discussed.

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