Journal Article

Modelling the interaction between relativistic and non-relativistic winds in the binary system PSR B1259−63/SS2883*– II. Impact of the magnetization and anisotropy of the pulsar wind

S. V. Bogovalov, D. Khangulyan, A. V. Koldoba, G. V. Ustyugova and F. A. Aharonian

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 419, issue 4, pages 3426-3432
Published in print February 2012 | ISSN: 0035-8711
Published online January 2012 | e-ISSN: 1365-2966 | DOI: https://dx.doi.org/10.1111/j.1365-2966.2011.19983.x
Modelling the interaction between relativistic and non-relativistic winds in the binary system PSR B1259−63/SS2883*– II. Impact of the magnetization and anisotropy of the pulsar wind

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In this paper, we present a numerical study of the properties of the flow produced by the collision of a magnetized anisotropic pulsar wind with its environment in a binary system. We compare the impact of both the magnetic field and the wind anisotropy with the benchmark case of a purely hydrodynamical (HD) interaction of isotropic winds, which has been studied in detail earlier. We consider the interaction in the axisymmetric approximation, that is, the pulsar rotation axis is assumed to be oriented along the line between the pulsar and the optical star, and the effects related to the pulsar orbiting are neglected. The impact of the magnetic field is studied for the case of weak magnetization (with magnetization parameter σ < 0.1), which is consistent with conventional models of pulsar winds. The effects related to anisotropy in pulsar winds are modelled assuming that the kinetic energy flux in a non-magnetized pulsar wind is strongly anisotropic, with the minimum at the pulsar rotation axis and the maximum in the perpendicular direction. We show that, although both considered effects change the shape of the region occupied by the terminated pulsar wind, their impact appears to be small. In particular, for the magnetization of the pulsar wind below 0.1, the magnetic field pressure remains well below the plasma pressure in the post-shock region. This is the opposite to what happens in prelions, that is, the pulsar interaction with the interstellar medium, where the magnetic field becomes dynamically important independently of the wind magnetization. Thus, in the case of the interaction of a pulsar with the stellar wind environment, the HD approach represents a feasible approximation for numerical modelling.

Keywords: hydrodynamics; MHD; shock waves; pulsars: general

Journal Article.  4644 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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