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PTP Online Top > Volume 94 (1995) > Number 6
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Prog. Theor. Phys. Vol. 94 No. 6 (1995) pp. 1001-1010

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(C + O) Star-Neutron Star Close Binary System Is a Progenitor of Soft Gamma-Ray Repeater?

Hitoshi Hanami, Takashi Nakamura* and Toshio Murakami**

Physics Section, Faculty of Humanities and Social Sciences, Iwate University, Morioka 020
*Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-01
**Institute of Space and Astronautical Sciences, Kanagawa 229

(Received July 28, 1995)

Abstract:

We consider a close binary system with separation ≃0.2 R⊙ which consists of a (C + O) star of mass ≃4 M⊙ and a neutron star as a progenitor of soft gamma-ray repeater (SGR) and a high velocity pulsar. The (C + O) star was tidally locked before the supernova explosion so that it has spin angular momentum large enough to be a rapidly rotating pulsar which will make a supernova remnant a plerion. After the event of the supernova explosion, both new and old neutron stars have high relative velocity of ≃1000 km s-1 to the center of mass of the ejecta. SGR activities can be induced by the episodic accretion of the supernova ejecta onto the old neutron star. The episodic accretion scenario onto the old neutron star predicts that SGR source should be located in the different position from the observed plerion-like object. Future observations with fine positional resolution can clarify the position ambiguity between the gamma ray and X-ray sources.


URL : http://ptp.ipap.jp/link?PTP/94/1001/
DOI : 10.1143/PTP.94.1001

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Citing Article(s) :

  1. Progress of Theoretical Physics Vol. 100 No. 5 (1998) pp. 921-929 :
    A Model for Non High Energy Gamma Ray Bursts and Sources of Ultra High Energy Cosmic Rays
    Takashi Nakamura
  2. Progress of Theoretical Physics Supplement No.143 (2001) pp. 50-77 :
    Jets and Central Engine of GRBs
    Takashi Nakamura

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