A new approach to the GeV flare of PSR B1259-63/LS2883

Abstract

PSR B1259-63/LS2883 is a binary system composed of a pulsar and a Be star. The Be star has an equatorial circumstellar disk (CD). The {\it Fermi} satellite discovered unexpected gamma-ray flares around 30 days after the last two periastron passages. The origin of the flares remain puzzling. In this work, we explore the possibility that, the GeV flares are consequences of inverse Compton-scattering of soft photons by the pulsar wind. The soft photons are from an accretion disk around the pulsar, which is composed by the matter from CD captured by the pulsar's gravity at disk-crossing before the periastron. At the other disk-crossing after the periastron, the density of the CD is not high enough so that accretion is prevented by the pulsar wind shock. This model can reproduce the observed SEDs and light curves satisfactorily.

arXiv comment14 pages, 8 figures, 1 table. Accepted for publication in ApJ

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Cited by in corpus (5)

• Modelling the multi-wavelength emissions from PSR B1259-63/LS 2883: the effects of the stellar disc on shock radiations
• The hour-timescale GeV flares of PSR B1259-63 in 2017
• The GeV emission of PSR B1259-63 during its last three periastron passages observed by Fermi-LAT
• On the timing behavior of PSR B1259-63 under the propeller torque from a transient accretion disc
• Probing the properties of the pulsar wind via studying the dispersive effects in the pulses from the pulsar companion in a double neutron-star binary system