Hostname: page-component-848d4c4894-cjp7w Total loading time: 0 Render date: 2024-07-05T21:37:00.013Z Has data issue: false hasContentIssue false
  • English
  • Français

Origin of High Velocity Pulsar and Soft Gamma Ray Repeaters

Published online by Cambridge University Press:  12 April 2016

Hitoshi Hanami
Hitoshi Hanami*
Affiliation:
Physics Section, College of Humanities and Social Sciences, Iwate University, Morioka 020, Japan

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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. After the event of the supernova explosion, both new and old neutron stars have high relative velocity of ≃ 1000km 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 or the strange high rotating pulsar of the new neutron star. Future observations with fine positional resolution can clarify the position ambiguity between the gamma ray and X-ray sources.

Type
Part 5 High Energy Phenomena
Information
International Astronomical Union Colloquium , Volume 160: Pulsars: Problems and Progress , 1996 , pp. 359 - 360
Copyright
Copyright © Astronomical Society of the Pacific 1996

References

Frail, D.A., Kulkarni, S.R. & Vasisht, G. 1993, Nature, 365, 136 Google Scholar
Hanami, H. et al. 1992, Prog. Theo. Phys., 94, 1001 Google Scholar
Kouveliotou, C. et al. 1994, Nature, 368, 125 Google Scholar
Kulkarni, S.R. & Frail, D.A. 1993, Nature, 365, 33 Google Scholar
Kulkarni, S.R. et al. 1994, Nature, 368, 129 Google Scholar
Yamaoka, H., Shigeyama, T. and Nomoto, K. 1993, A&A, 267, 433 Google Scholar