Hostname: page-component-586b7cd67f-t7fkt Total loading time: 0 Render date: 2024-11-23T17:32:16.360Z Has data issue: false hasContentIssue false
  • English
  • Français

Explosion of very massive stars and the origin of intermediate mass black holes

Published online by Cambridge University Press:  01 August 2006

Sachiko Tsuruta ,
Takuya Ohkubo ,
Hideyuki Umeda ,
Keiichi Maeda ,
Ken'ichi Nomoto ,
Tomoharu Suzuki  and
Martin J. Rees
Sachiko Tsuruta
Affiliation:
Department of Physics, Montana State University, Bozeman, MT 59717, USA email: [email protected]
Takuya Ohkubo
Affiliation:
Department of Astronomy, Univ. of Tokyo, Hongo, Bunkyo-ku, Tokyo, Japan email: [email protected], [email protected], [email protected]
Hideyuki Umeda
Affiliation:
Department of Astronomy, Univ. of Tokyo, Hongo, Bunkyo-ku, Tokyo, Japan email: [email protected], [email protected], [email protected]
Keiichi Maeda
Affiliation:
Department of Earth Sci. and Astron., Univ. of Tokyo, Komaba, Meguro-ku, Tokyo, Japan email: [email protected]
Ken'ichi Nomoto
Affiliation:
Department of Astronomy, Univ. of Tokyo, Hongo, Bunkyo-ku, Tokyo, Japan email: [email protected], [email protected], [email protected] Research Center for the Early Universe, Univ. of Tokyo, Hongo, Bunkyo-ku, Tokyo, Japan email: [email protected]
Tomoharu Suzuki
Affiliation:
Department of Astronomy, Univ. of Tokyo, Hongo, Bunkyo-ku, Tokyo, Japan email: [email protected], [email protected], [email protected]
Martin J. Rees
Affiliation:
Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge 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, collapse, explosion, and nucleosynthesis of Population III very massive stars with 500 M⊙ and 1000 M⊙. It was found that both 500 M⊙ and 1000 M⊙ models enter the region of pair-instability but continue to undergo core collapse to black holes. For moderately aspherical explosions, the patterns of nucleosynthesis match the observational data of intergalactic and intercluster medium and hot gases in M82, better than models involving hypernovae and pair instability supernovae.

Our results suggest that explosions of Population III core-collapse very massive stars contribute significantly to the chemical evolution of gases in clusters of galaxies. The final black hole masses are about 500 M⊙ for our most massive 1000 M⊙ models. This result may support the view that Population III very massive stars are responsible for the origin of intermediate mass black holes which were recently reported to be discovered.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S238: Black Holes from Stars to Galaxies – Across the Range of Masses , August 2006 , pp. 241 - 246
Copyright
Copyright © International Astronomical Union 2007

References

Abel, T., Bryan, G. L. & Norman, M. L. 2000, ApJ, 540, 39CrossRefGoogle Scholar
Bromm, V., Coppi, P. S. & Larson, R. B. 2002, ApJ, 564, 23CrossRefGoogle Scholar
Bromm, V., Kudritzki, R. P. & Loeb, A. 2001, ApJ, 552, 464CrossRefGoogle Scholar
Bromm, V. & Loeb, A. 2004, NewA, 9, 353Google Scholar
Ebisuzaki, T., Makino, J., Tsuru, T. G., Funato, Y., Portegies Zwart, S., Hut, P. et al. 2001, ApJ, 562, L19Google Scholar
Fryer, C. L., Woosley, S. E. & Heger, A. 2001, ApJ, 550, 372Google Scholar
Gnedin, N. Y. & Ostriker, J. P. 1997, ApJ, 486, 581CrossRefGoogle Scholar
Heger, A. & Woosley, S. E. 2002, ApJ, 567, 532CrossRefGoogle Scholar
Kogut, A., Spergel, D. N., Barnes, C., Bennett, C. L., Halpern, M. & Hinshaw, G. et al. 2003, ApJS, 148, 161CrossRefGoogle Scholar
Kormendy, J. & Richstone, D. 1995, ARA&A, 33, 581Google Scholar
Ohkubo, T., Umeda, H., Maeda, K., Nomoto, K., Suzuki, T., Tsuruta, S. et al. 2006, ApJ, 645, 1352 (O06)CrossRefGoogle Scholar
Omukai, K. & Palla, F. 2003, ApJ, 589, 677CrossRefGoogle Scholar
Portegies, Zwart, S. F.Baumgardt, H.Hut, P.Makino, J. & McMillan, S. L. W. 2004, Nature, 428, 724Google Scholar
Qian, Y.-Z., Sargent, W. L. W. & Wasserburg, G. J. 2002, ApJ, 588, 1099Google Scholar
Tumlinson, J., Venkatesen, A. & Shull, J. M. 2004, ApJ, 612, 602CrossRefGoogle Scholar
Umeda, H. & Nomoto, K. 2002, ApJ, 565, 385Google Scholar
Umeda, H. & Nomoto, K. 2003, Nature, 422, 871CrossRefGoogle Scholar
Venkatesan, A., Tumlinson, J. & Shull, J. M. 2003, ApJ, 584, 621Google Scholar
Venkatesan, A. & Truran, J. W. 2003, ApJ, 594, L1CrossRefGoogle Scholar