Hostname: page-component-78c5997874-94fs2 Total loading time: 0 Render date: 2024-11-19T07:13:18.645Z Has data issue: false hasContentIssue false
  • English
  • Français

Population III Very-Massive Stars—Their Evolution and Explosion

Published online by Cambridge University Press:  23 December 2005

Takuya Ohkubo ,
H. Umeda ,
K. Maeda ,
K. Nomoto ,
S. Tsuruta  and
M.J. Rees
Takuya Ohkubo
Affiliation:
Department of Astronomy, University of Tokyo, 7-3-1 Hongo Bunkyo-ku, Tokyo, Japan email: [email protected], [email protected], [email protected]
H. Umeda
Affiliation:
Department of Astronomy, University of Tokyo, 7-3-1 Hongo Bunkyo-ku, Tokyo, Japan email: [email protected], [email protected], [email protected]
K. Maeda
Affiliation:
Department of Earth Science and Astronomy, University of Tokyo, 3-8-1 Komaba, Meguro-ku, Tokyo, Japan email: [email protected]
K. Nomoto
Affiliation:
Department of Astronomy, University of Tokyo, 7-3-1 Hongo Bunkyo-ku, Tokyo, Japan email: [email protected], [email protected], [email protected]
S. Tsuruta
Affiliation:
Department of Physics, Montana State University, Bozeman, MT 59717-3840, USA email: [email protected]
M.J. Rees
Affiliation:
Institute of Astronomy, Cambridge University, Madingley Road, Cambrigde CB3 0HA, UK email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We calculate evolution, explosion and nucleosynthesis of 1000$M_{\odot}$ stars. Even such massive stars may explode at the end of their lives if they rotate. We use a 2 dimensional hydrodynamical code to take aspherisity by the effect of rotation into account. Our results show that (1) abundance pattern of ejected matter by explosion is consistent with observational data of intracluster medium gas and M82 hot gas, (2) such massive stars can supply more efficient UV photons to re-ionize HI, HeI and HeII than ordinary massive stars (less than 100 solar-masses) and (3) final black hole mass is 500 solar-mass, which is consistent of the mass scale of intermediate-mass black hole (IHBH) found in M82.

Keywords

Nuclear reactionsnucleosynthesisabundances – stars: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S228: From Lithium to Uranium: Elemental Tracers of Early Cosmic Evolution , May 2005 , pp. 167 - 168
Copyright
© 2005 International Astronomical Union