Star SS2883 in what follows will be referred to as LS2883 according to the standard catalogue of Luminous Stars in the Southern Milky Way (Stephenson & Sanduleak 1971).
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★
Version of Record online: 28 NOV 2011
© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS
Monthly Notices of the Royal Astronomical Society
Volume 419, Issue 4, pages 3426–3432, February 2012
How to Cite
Bogovalov, S. V., Khangulyan, D., Koldoba, A. V., Ustyugova, G. V. and Aharonian, F. A. (2012), 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. Monthly Notices of the Royal Astronomical Society, 419: 3426–3432. doi: 10.1111/j.1365-2966.2011.19983.x
- Issue online: 9 JAN 2012
- Version of Record online: 28 NOV 2011
- Accepted 2011 October 11. Received 2011 October 5; in original form 2011 July 14
- shock waves;
- pulsars: general
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.