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On the Origin of Hyperfast Neutron Stars

Published online by Cambridge University Press:  01 September 2007

V.V. Gvaramadze ,
A. Gualandris  and
S. Portegies Zwart
V.V. Gvaramadze
Affiliation:
Sternberg Astronomical Institute, Moscow State University, Universitetskij Pr. 13, Moscow 119992, Russia email: vgvaram@mx.iki.rssi.ru
A. Gualandris
Affiliation:
Center for Computational Relativity and Gravitation, Rochester Institute of Technology, 78 Lomb Memorial Drive, Rochester, NY14623, USA email: alessiag@astro.rit.edu Astronomical Institute ‘Anton Pannekoek’ and Section Computational Science, Amsterdam University, Kruislaan 403, 1098 SJ, Amsterdam, the Netherlands email: spz@science.uva.nl
S. Portegies Zwart
Affiliation:
Astronomical Institute ‘Anton Pannekoek’ and Section Computational Science, Amsterdam University, Kruislaan 403, 1098 SJ, Amsterdam, the Netherlands email: spz@science.uva.nl
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Abstract

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We propose an explanation for the origin of hyperfast neutron stars (e.g. PSR B1508+55, PSR B2224+65, RX J0822–4300) based on the hypothesis that they could be the remnants of a symmetric supernova explosion of a high-velocity massive star (or its helium core) which attained its peculiar velocity (similar to that of the neutron star) in the course of a strong three- or four-body dynamical encounter in the core of a young massive star cluster. This hypothesis implies that the dense cores of star clusters (located either in the Galactic disk or near the Galactic centre) could also produce the so-called hypervelocity stars – ordinary stars moving with a speed of ~ 1 000 km s−1.

Keywords

Stars: neutronpulsars: generalpulsars: individual (B1508+55)galaxies: star clustersmethods: n-body simulationss
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S246: Dynamical Evolution of Dense Stellar Systems , September 2007 , pp. 365 - 366
Copyright
Copyright © International Astronomical Union 2008

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