楕円銀河の高温ガスの熱源としてのIa型超新星(宇宙の階層構造,研究会報告)

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概要

• 論文の詳細を見る

• We present a stationary and thermally stable model for X-ray emitting gases of elliptical galaxies. In this model, the gas is mainly heated by type Ia supernovae and the thermal conduction from the hotter intracluster gas. Thermal conduction stabilizes the gas close to the center even when the temperature of the gas thereof becomes as low as 1 keV. The gas is cooled down mainly due to line emissions from heavy elements. As an example, we show that this model can reproduce the temperature and density distributions of the cD galaxy M87 in the Virgo cluster obtained from the observations by an X-ray satellite ASCA. We also investigate emission lines from type Ia supernova remnants (SNRs) in elliptical galaxies, because this is important for determining abundances in the halo gas of elliptical galaxies. As a result, it is found that the ejecta mainly composed of iron stalls to make a hot bubble in 〜 10^6 years after explosion due to the high pressure of the surrounding medium. The size of the ejecta is about 1 pc. These ejecta emit only 〜 7×10^<30> erg s^<-1> of Fe L emission lines per supernova due to the high temperature and low density.

• 1996-06-20

著者

• 茂山 俊和

  東京大理

• 茂山 俊和

  東大理

• Saitoh R.

  Department of Astronomy, School of Science, University of Tokyo

• Fujita Y.

  Yukawa Institute of Physics, Kyoto University

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