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Thermal X-Rays due to Ejecta/CSM Interaction in SN 1987A

Published online by Cambridge University Press:  12 April 2016

K. Masai ,
S. Hayakawa ,
H. Itoh ,
K. Nomoto  and
T. Shigeyama
K. Masai
Affiliation:
Institute of Plasma Physics, Nagoya University, Nagoya 464, Japan
S. Hayakawa
Affiliation:
Department of Astrophysics, Nagoya University, Nagoya 464, Japan
H. Itoh
Affiliation:
Department of Astronomy, University of Kyoto, Kyoto 606, Japan
K. Nomoto
Affiliation:
Department of Earth Science and Astronomy, University of Tokyo, Tokyo 153, Japan
T. Shigeyama
Affiliation:
Department of Earth Science and Astronomy, University of Tokyo, Tokyo 153, Japan

Extract

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The X-ray spectrum observed by Ginga is characterized by a component below 10keV which decreases with increasing photon energy, and a component above 10keV which is nearly flat. This unusual X-ray spectrum may be understood as follows; X-rays below 10keV is likely to be due to thermal emission coming from the shock-heated ejecta, and X-rays above 10keV to be due to γ-ray degradation inside the ejecta. If thermal emission due to the collision of the ejecta with circumstellar matter (CSM) is responsible for X-rays below 10keV, the epoch of the collision can be estimated to be ∼ 0.2yr after the explosion if ∼ 0.5yr is the time when the X-ray flux at ∼ 10keV reaches its maximum. The X-ray light curve then requires the inner radius of CSM to be ∼ 1×1016cm for an expansion velocity, Vex ≃2×109cm s−1.

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. 450 - 451
Copyright
Copyright © Springer-Verlag 1988

References

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5) Itoh, M., Kumagai, S., Shigeyama, T., Nomoto, K., and Nishimura, J., Nature 330, 233–235 (1987), and references therein.CrossRefGoogle Scholar