Volume 627, July 2019
|Number of page(s)||10|
|Published online||04 July 2019|
Modelling multiwavelength emissions from PSR B1259–63/LS 2883: Effects of the stellar disc on shock radiations
Institute of Astrophysics, Central China Normal University, Wuhan 430079, PR China
2 Department of Physics, The University of Hong Kong, Pokfulam Road, Hong Kong
3 School of Physics, Huazhong University of Science and Technology, Wuhan 430074, PR China
4 Department of Astrophysics, Radboud University Nijmegen, PO Box 9010 6500 GL Nijmegen, The Netherlands
Accepted: 11 April 2019
PSR B1259–63/LS 2883 is an elliptical pulsar/Be star binary that emits broadband emissions from radio to TeV γ-rays. The massive star possesses an equatorial disc that is inclined with the orbital plane of the pulsar. Non-thermal emission from the system is believed to be produced by pulsar wind shock and double-peak profiles in the X-ray, and TeV γ-ray light curves are related to the phases of the pulsar passing through the disc region of the star. In this paper, we investigate the interactions between the pulsar wind and stellar outflows, especially with the presence of the disc, and present a multiwavelength modelling of the emission from this system. We show that the double-peak profiles of X-ray and TeV γ-ray light curves are caused by the enhancements of the magnetic field and soft photons at the shock during the disc passages. As the pulsar is passing through the equatorial disc, the additional pressure of the disc pushes the shock surface closer to the pulsar, which causes the enhancement of magnetic field in the shock, and thus increases the synchrotron luminosity. The TeV γ-rays due to the inverse-Compton (IC) scattering of shocked electrons with seed photons from the star are expected to peak around periastron, which is inconsistent with observations. However, the shock heating of the stellar disc could provide additional seed photons for IC scattering during the disc passages, and thus produces the double-peak profiles as observed in the TeV γ-ray light curve. Our model can possibly be examined and applied to other similar gamma-ray binaries, such as PSR J2032+4127/MT91 213, HESS J0632+057, and LS I+61°303.
Key words: binaries: close / X-rays: binaries / gamma rays: stars / pulsars: individual: PSR B1259–63
© ESO 2019
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