新しいタイプの超新星とそのモデル(中性子星の構造と進化,研究会報告)
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概要
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Using flux-calibrated spectra, we construct aquasibolometric (3280-9100 Å) light curve of the type Ic ("helium-poor Ib") supernova 1987M. This light curve has two important features that are difficult to understand in the context of previous Wolf-Rayet progenitor models: (1) Near maximum brightness, SN 1987M was only about 0.6 mag dimmer than type Ia supernovae, significantly brighter than typical type Ib supemovae. (2) The brightness of SN 1987M fell more rapidly than that of type la and Ib supemovae. We present a theoretical light curve of an exploding 3.3 M_⊙ helium star which, in contrast to the previous models, is in good agreement with the observed light curve of SN 1987M. We argue that SN 1987M may have been the explosion of a helium star of 3-3.5 M_⊙ that began its life with 12-15 M_⊙ in a close binary system and gradually lost its mass to the companion.
- 素粒子論グループ 素粒子研究編集部の論文
- 1991-03-20
著者
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野本 憲一
Department Of Astronomy And Research Center For The Early Universe The University Of Tokyo
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Shigeyama T.
Department Of Astronomy Faculty Of Science University Of Tokyo:max-planck-institut Fur Physik Und As
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Nomoto K.
Department Of Astronomy Faculty Of Science University Of Tokyo:max-planck-institut Fur Physik Und As
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Filippenko A.
Department of Astronomy, and Center for Particle Astrophysics, University of California
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Filippenko A.
Department Of Astronomy And Center For Particle Astrophysics University Of California
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