Physics of accretion onto young stars. II. Structure and evolution of accreting stars.

Details Physics of accretion onto young stars. II. Structure and evolution of accreting stars. Physics of accretion onto young stars. II. Structure and evolution of accreting stars.

Oct 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...326.1001s&link_type=abstract

Astronomy and Astrophysics, v.326, p.1001-1012

Astronomy and Astrophysics

Astrophysics

34

Accretion, Pre-Main Sequence Stars, Stellar Evolution, Hertzsprung-Russell (Hr) Diagram

Scientific paper

We present new computations of pre-main sequence evolution for stars that accrete a substantial part of their mass. We compute several models with different mass accretion rates, focusing on the effect of deuterium burning on stellar evolution during the accretion phase. We treat accretion not only as a surface boundary condition but as a global phenomenon that affect also the inner parts of the star, using a formalism developed by Siess & Forestini (1996A&A...308..472S). We study the effect of varying the mass distribution of accreted matter into the star, and analyze the influence of different chemical compositions for the accreted matter. We also take into account the possible deposition of accretion energy transported by the accreted matter. We show that accretion can lead to substantial changes in the pre-main sequence evolutionary tracks in the Hertzsprung-Russell diagram (HRD). When accretion stops, the star relaxes to its ``standard'' track in the HRD, and this, independently of the previous accretion rate.

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