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A Rotating Stellar Collapse Model for Supernova 1987a

Published online by Cambridge University Press:  12 April 2016

Takashi Nakamura  and
Masataka Fukugita
Takashi Nakamura
Affiliation:
Department of Physics, Kyoto University, Kyoto 606, Japan
Masataka Fukugita
Affiliation:
Research Institute for Fundamental Physics , Kyoto University, Kyoto 606, Japan

Extract

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It is shown that the bunch structure of the Kamiokande neutrino events associated with SN1987a can be naturally understood, if one assumes that the core of the progenitor star was rotating moderately with q(≡ Jc/GM2) ≈ 3 with J the total angular momentum and M the gravitational mass of the core.

We assume that the presence of the observed gap, at least that between the second and the third bunch, is real and consider its implications in the dynamics of the core collapse. Let us define a nondimensional angular momentum q(≡ Jc/GM2) with J the total angular momentum and M the gravitational mass of the core. We assume that the value of q for the core of SN1987a was about 3. Then we expect that the effect of the angular momentum plays an important role when the size of the core r shrinks to < 107cm. In the spherically symmetric collapse model, the size of the unshocked homologous core is of the order of 107cm. Hence we expect that the core at the bounce is essentially governed by the spherically symmetric dynamics. To verify this point we may refer to the simulation by Symbalisty1. Our model almost corresponds to Model ROT2 in which one obtains a neutrinosphere with a roughly spherical radius of approximately 50km. We then expect that the infalling nonhomologous matter onto the core will liberate a gravitational energy of the order of 1052ergs.

Type
Part III. Chemical and Dynamical Structures of Exploding Stars
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 432 - 433
Copyright
Copyright © Springer-Verlag 1988

References

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