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Primordial stellar evolution - The pre-main-sequence phaseThe quasi-static contraction of primordial stars composed of pure hydrogen and helium gas is studied by following numerically the evolution of a star of five solar masses 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. Deuterium later ignites at an off-center temperature maximum but fails to produce interior convection. The star follows a conventional premain sequence track in the HR diagram, reaching the ZAMS after 1.2 million yr, with a luminosity of 880 solar luminosities and a radius of 1.2 solar radii.
Document ID
19870032200
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Stahler, S. W.
(Harvard-Smithsonian Center for Astrophysics; MIT Cambridge, MA, United States)
Palla, F.
(Arcetri Osservatorio Astrofisico, Florence, Italy)
Salpeter, E. E.
(Cornell University Ithaca, NY, United States)
Date Acquired
August 13, 2013
Publication Date
September 15, 1986
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 308
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
87A19474
Funding Number(s)
CONTRACT_GRANT: NSF AST-84-15162
CONTRACT_GRANT: NAGW-246
Distribution Limits
Public
Copyright
Other

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