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On the Central Engine of Short Gamma-ray Bursts

Published online by Cambridge University Press:  19 September 2016

Stephan Rosswog  and
Enrico Ramírez-Ruiz
Stephan Rosswog
Affiliation:
Dept. Physics & Astronomy, University of Leicester, Leicester LEI 7RH, UK; [email protected]
Enrico Ramírez-Ruiz
Affiliation:
Institute of Astronomy, Cambridge, CB3 OHA, UK; [email protected]

Summary

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We assess the ability of neutron star binary coalescence to produce short gamma-ray bursts (GRBs). We find that the neutrino annihilation above the merged remnant will drive bipolar, relativistic jets along the initial binary rotation axis. This outflow can be collimated by the energetic, neutrino-driven baryonic wind that is blown off the remnant. Despite the narrow neutron star mass distribution the apparent luminosities will be spread over a broad range from ~ 1049 to ~ 1052erg s−1, typical jet opening half-angles are around 5 degrees. If the central core of the merger remnant does not collapse immediately convective dynamo action will set in and the available kinetic energy can be transformed into magnetic fields in excess of 1017 G. The corresponding spin-down time scale is ~ 0.2 s, just about the duration of a short GRB.

Type
Part VII Gamma-Ray Bursters
Information
International Astronomical Union Colloquium , Volume 192: Cosmic Explosions , 2005 , pp. 503 - 508
Copyright
Copyright © Springer-Verlag 2005

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