HESS J0632+057: hydrodynamics and non-thermal emission. (2nd August 2017)

• Record Type: Journal Article
• Authors: Bosch-Ramon, Valentí; Barkov, Maxim V.; Mignone, Andrea; Bordas, Pol
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 471:Number 1(2017:Oct.)
• Page Start: L150
• Page End: L154
• Publication Date: 2017-08-02
• Subjects: hydrodynamics -- radiation mechanisms: non-thermal -- stars: winds, outflows -- gamma-rays: stars -- X-rays: binaries; Astronomy -- Research -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnrasl/slx124
• Languages: English
• ISSNs: 1745-3933

Abstract

Abstract: HESS J0632+057 is an eccentric gamma-ray Be binary that produces non-thermal radio, X-rays, GeV and very high-energy gamma-rays. The non-thermal emission of HESS J0632+057 is modulated with the orbital period, with a dominant maximum before apastron passage. The nature of the compact object in HESS J0632+057 is not known, although it has been proposed to be a young pulsar as in PSR B1259–63, the only gamma-ray emitting high-mass binary known to host a non-accreting pulsar. In this letter, we present hydrodynamical simulations of HESS J0632+057 in the context of a pulsar and a stellar wind interacting in an eccentric binary, and propose a scenario for the non-thermal phenomenology of the source. In this scenario, the non-thermal activity before and around apastron is linked to the accumulation of non-thermal particles in the vicinity of the binary, and the sudden drop of the emission before apastron is produced by the disruption of the two-wind interaction structure, allowing these particles to escape efficiently. In addition to providing a framework to explain the non-thermal phenomenology of the source, this scenario predicts extended, moving X-ray emitting structures similar to those observed in PSR B1259–63.