Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001apj...561l..55o&link_type=abstract
The Astrophysical Journal, Volume 561, Issue 1, pp. L55-L58.
Astronomy and Astrophysics
Astronomy
55
Cosmology: Theory, Cosmology: Early Universe, Stars: Formation, Stars: Pre-Main-Sequence
Scientific paper
We investigate the formation by accretion of massive primordial protostars in the range of 10-300 Msolar. The high accretion rate used in the models (M=4.4×10-3 Msolar yr-1) causes the structure and evolution to differ significantly from those of both present-day protostars and primordial zero-age main-sequence stars. After an initial expansion of the radius (for M*<~12 Msolar), the protostar undergoes an extended phase of contraction (up to M*~=60 Msolar). The stellar surface is not visible throughout most of the main accretion phase since a photosphere is formed in the infalling envelope. Also, significant nuclear burning does not take place until a protostellar mass of about 80 Msolar is reached. As the interior luminosity approaches the Eddington luminosity, the protostellar radius rapidly expands, reaching a maximum at around 100 Msolar. Changes in the ionization of the surface layers induce a secondary phase of contraction, followed by a final swelling due to radiation pressure when the stellar mass reaches about 300 Msolar. This expansion is likely to signal the end of the main accretion phase, thus setting an upper limit to the protostellar mass formed in these conditions.
Omukai Kazuyuki
Palla Francesco
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