Modeling interaction of relativistic and nonrelativistic winds in binary system PSR 1259-63/SS2883. I.Hydrodynamical limit

Abstract

In this paper, we present a detailed hydrodynamical study of the properties of the flow produced by the collision of a pulsar wind with the surrounding in a binary system. This work is the first attempt to simulate interaction of the ultrarelativistic flow (pulsar wind) with the nonrelativistic stellar wind. Obtained results show that the wind collision could result in the formation of an "unclosed" (at spatial scales comparable to the binary system size) pulsar wind termination shock even when the stellar wind ram pressure exceeds significantly the pulsar wind kinetical pressure. Moreover, the post-shock flow propagates in a rather narrow region, with very high bulk Lorentz factor ($\gamma \sim 100$). This flow acceleration is related to adiabatical losses, which are purely hydrodynamical effects. Interestingly, in this particular case, no magnetic field is required for formation of the ultrarelativistic bulk outflow. The obtained results provide a new interpretation for the orbital variability of radio, X-ray and gamma-ray signals detected from binary pulsar system PSR 1259-63/SS2883.

11 pages, 13 figures, submitted to MNRAS

References in corpus (4)

• Accretion vs colliding wind models for the gamma-ray binary LS I +61 303: an assessment
• Three-dimensional hydrodynamic simulations of asymmetric pulsar wind bow shocks
• The 2000 Periastron Passage of PSR B1259-63
• Hadronic model for radio-to-TeV gamma-ray emission from PSR B1259-63

Cited by in corpus (6)

• Understanding the Very High-Energy Emission from Microquasars
• A 3D dynamical model of the colliding winds in binary systems
• The magnetic field and the location of the TeV emitter in Cygnus X-1 and LS 5039
• Probing the Pulsar Wind in the gamma-ray Binary System PSR B1259-63/SS 2883
• Studying the properties of the radio emitter in LS 5039
• LS I+61 303: microquasar or not microquasar?