Physics of accretion onto young stars. III. Comparisons with observations

Details Physics of accretion onto young stars. III. Comparisons with observations Physics of accretion onto young stars. III. Comparisons with observations

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...342..480s&link_type=abstract

Astronomy and Astrophysics, v.342, p.480-491 (1999)

Astronomy and Astrophysics

Astrophysics

41

Accretion, Accretion Disks, Stars: Abundances, Stars: Evolution, Stars: Fundamental Parameters, Stars: Pre-Main Sequence

Scientific paper

We present new evolutionary sequences for long lasting accreting low-mass (0.1 M_sun <= M <= 2.5 M_sun ) pre-main sequence stars. The calculations, performed for two different mass accretion rates, show that accretion accelerates the evolution of the star. The star has a smaller radius and goes down its convective track faster than in a standard scheme. Consequently, the age of a star, as given by its location on the Hertzsprung-Russell diagram, is lower than that of a non-accreting star. We discuss (2) H and (7) Li burning and show how accretion affects the surface abundance of these elements. Notably, we point out that deuterium must be present at the surface of accreting intermediate-mass stars. Finally, we estimate the age, mass and radius of a sample of T Tauri stars located in the Taurus Auriga star forming region.

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