Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...375..288p&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 375, July 1, 1991, p. 288-299.
Astronomy and Astrophysics
Astrophysics
100
Pre-Main Sequence Stars, Protostars, Star Formation, Stellar Evolution, Stellar Interiors, Stellar Structure, Deuterium, Herbig-Haro Objects, Stellar Luminosity, Stellar Mass Accretion
Scientific paper
A numerical calculation of the structure and evolution of Population I protostars in the range from 1 to 8 solar masses is presented. The protostar is modeled as being built up from a spherically symmetric accretion flow, with a constant mass accretion rate of 0.00001 solar mass/yr. The protostar is initially fully convective due to the steady state burning of deuterium near its center. The mass-radius relation during this phase is derived analytically. At 2.4 solar masses, a radiative barrier appears which prevents the convective transport of deuterium to the center. The subsurface shell is ignited by the deuterium, which causes the protostar to swell. The star joins the zero-age main sequence by the time it reaches 8 solar masses. It is found that over a significant mass range, protostars contain a substantial amount of deuterium, and it is inferred that the ignition of this fuel during subsequent premain-sequence contraction could drive the surface convection that is apparently present in many Herbig Ae and Be stars.
Palla Francesco
Stahler Steven W.
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