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Black Hole Disk Accretion in Supernovae

Published online by Cambridge University Press:  25 May 2016

H. Nomura ,
S. Mineshige ,
M. Hirose ,
K. Nomoto  and
T. Suzuki
H. Nomura
Affiliation:
Department of Astronomy, Faculty of Science, Kyoto University, Sakyo-ku, Kyoto 606-01, Japan
S. Mineshige
Affiliation:
Department of Astronomy, Faculty of Science, Kyoto University, Sakyo-ku, Kyoto 606-01, Japan
M. Hirose
Affiliation:
Theoretical Physics, Astronomical Observatory of Japan, Japan
K. Nomoto
Affiliation:
Department of Astronomy and Research Center for the Early Universe, School of Science, University of Tokyo, Japan
T. Suzuki
Affiliation:
Department of Astronomy and Research Center for the Early Universe, School of Science, University of Tokyo, Japan

Extract

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Massive stars in a certain mass range (20 – 40M⊙) may form low mass black holes after supernova explosions. In such massive stars, fall back of ~ 0.1M⊙ materials onto a black hole is expected due to a deep gravitational potential or a reverse shock propagating back from the outer composition interface. We study hydrodynamical disk accretion onto a new-born low mass black hole in a supernova using the SPH (Smoothed Particle Hydrodynamics) method.

Type
Session 1: Plasma and Fresh Nucleosynthesis Phenomena
Information
Symposium - International Astronomical Union , Volume 188: The Hot Universe , 1998 , pp. 243 - 244
Copyright
Copyright © Kluwer 1998 

References

Mineshige, S., Nomura, H., Hirose, M., Nomoto, K., & Suzuki, T. (1997) ApJ , 489, 227 CrossRefGoogle Scholar