TY - JOUR
T1 - On the formation of massive primordial stars
AU - Omukai, Kazuyuki
AU - Palla, Francesco
N1 - Funding Information:
This work is supported in part by Research Fellowships of the Japan Society for the Promotion of Science for Young Scientists, grant 6819. K. O. wishes to thank the director of the Osservatorio di Arcetri for the hospitality received during an extended visit in 2001.
Publisher Copyright:
© 2001. The American Astronomical Society.
PY - 2001/11/1
Y1 - 2001/11/1
N2 - We investigate the formation by accretion of massive primordial protostars in the range of 10-300 M· The , high accretion rate used in the models (M=4.4×10-3M·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. ≤ 12M·), the protostar undergoes an extended phase of contraction (up to M. ≃60 M·). 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 M, is reached. As the interior luminosity approaches the Eddington luminosity, the protostellar radius rapidly expands, reaching a maximum at around 100 M·. 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 M·. 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.
AB - We investigate the formation by accretion of massive primordial protostars in the range of 10-300 M· The , high accretion rate used in the models (M=4.4×10-3M·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. ≤ 12M·), the protostar undergoes an extended phase of contraction (up to M. ≃60 M·). 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 M, is reached. As the interior luminosity approaches the Eddington luminosity, the protostellar radius rapidly expands, reaching a maximum at around 100 M·. 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 M·. 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.
KW - Cosmology: Theory-early Universe-stars: Formation-stars: Pre-main-Sequence
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U2 - 10.1086/324410
DO - 10.1086/324410
M3 - Article
AN - SCOPUS:85033485234
VL - 561
SP - L35-L58
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
SN - 2041-8205
IS - 1
ER -