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Two-dimensional numerical study for relativistic outflow from strongly magnetized neutron stars

Published online by Cambridge University Press:  01 November 2008

Jin Matsumoto ,
Youhei Masada ,
Eiji Asano  and
Kazunari Shibata
Jin Matsumoto
Affiliation:
Kwasan and Hida Observatories, Kyoto University, Kyoto, Japan email: [email protected] Department of Astronomy, Kyoto University, Kyoto, Japan.
Youhei Masada
Affiliation:
Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan, R.O.C.
Eiji Asano
Affiliation:
Kwasan and Hida Observatories, Kyoto University, Kyoto, Japan email: [email protected]
Kazunari Shibata
Affiliation:
Kwasan and Hida Observatories, Kyoto University, Kyoto, Japan email: [email protected]
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Abstract

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Using special relativistic magnetohydrodynamic simulation, the nonlinear dynamics of the magnetized outflow triggered on the magnetar surface is investigated. It is found that the strong shock propagates in the circumstellar medium in association with the expanding outflow. The shock velocity vsh depends on the strength of the dipole field anchored to the stellar surface Bdipole and is described by a simple scaling relation vsh ∝ Bdipole0.5. In addition, the outflow-driven shock can be accelerated self-similarly to the relativistic velocity when the density profile of the circumstellar medium is steeper than the critical density profile, that is α ≡ d logρ(r)/d log r ≲ αcrit = −5.0, where the density is set as a power law distribution with an index α and r is the cylindrical radius. Our results suggest that the relativistic outflow would be driven by the flaring activity in a circumstellar medium with a steep density profile.

Keywords

Relativity – MHD – stars: neutron – methods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S259: Cosmic Magnetic Fields: From Planets, to Stars and Galaxies , November 2008 , pp. 139 - 140
Copyright
Copyright © International Astronomical Union 2009

References

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