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Large solar-type magnetic reconnection model for magnetar giant flare

  • Youhei Masada (a1)

Abstract

We construct a magnetic reconnection model for magnetar giant flare in the framework of solar flare/coronal mass ejection theory. As is the case with the solar flare, the explosive magnetic reconnection plays a crucial role in the energetics of the magnetar flare. A key physics controlling the energy transport in the system, on the other hand, is the radiative process unlike that in the solar flare. After the release of the magnetic energy via the magnetic reconnection, the radiative heat flux drives the baryonic evaporation. Our model can predict that the baryonic matter evaporated in the preflare stage would be the origin of the radio emitting ejecta observed in association with the giant flare on 2004 December 27 from SGR1806-20.

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Copyright

References

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Lyutikov, M. 2006, MNRAS 367, 1594
Masada, Y., Nagataki, S., Shibata, K., & Terasawa, T. 2008, arXiv:0803.3818
Shibata, K. & Yokoyama, T. 1999, ApJL 526, L49
Thompson, C. & Duncan, R. C. 1995, MNRAS 275, 255
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Large solar-type magnetic reconnection model for magnetar giant flare

  • Youhei Masada (a1)

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