Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...308..697s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 308, Sept. 15, 1986, p. 697-705. CNR-supported research.
Astronomy and Astrophysics
Astrophysics
15
Pre-Main Sequence Stars, Protostars, Star Formation, Stellar Evolution, Stellar Models, Mass To Light Ratios, Red Shift, Spiral Galaxies, Stellar Cores, Stellar Mass Accretion
Scientific paper
The authors consider the quasi-static contraction of primordial stars composed of pure hydrogen and helium gas. They follow numerically the evolution of a star of mass M* = 5 M_sun; from the end of protostellar accretion to the onset of hydrogen burning. Although the protostellar core of this mass is radiatively stable and undergoing nonhomologous contraction, its large surface area and luminosity force the star to a partially convective, homologously contracting state within only 100 yr. The star follows a conventional pre-main-sequence track in the H-R diagram, reaching the zero-age main sequence after 1.2×106yr, with a luminosity of 880 L_sun; and a radius of 1.2 R_sun;. All stars with M* < 7 M_sun; undergo a similar rapid relaxation to homologous contraction because of their large initial radii and surface luminosities.
Palla Fabrizio
Salpeter Edwin E.
Stahler Steven W.
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