Modeling the multi-wavelength light curves of PSR B1259-63/SS 2883

TL;DR

This paper develops a shocked wind model with variable magnetic parameters to explain multi-wavelength light curves of PSR B1259-63/SS 2883, successfully reproducing observed features across X-ray and TeV bands.

Contribution

It introduces a new model incorporating magnetic parameter variation to explain multi-wavelength emissions in the binary system.

Findings

Model reproduces two-peak X-ray and TeV light curves.

Effect of the stellar disk causes emission and absorption features.

Doppler boosting may produce GeV flares.

Abstract

PSR B1259-63/SS 2883 is a binary system in which a 48-ms pulsar orbits around a Be star in a high eccentric orbit with a long orbital period of about 3.4 yr. Extensive broadband observational data are available for this system from radio band to very high energy (VHE) range. The multi-frequency emission is unpulsed and nonthermal, and is generally thought to be related to the relativistic electrons accelerated from the interaction between the pulsar wind and the stellar wind, where X-ray emission is from the synchrotron process and the VHE emission is from the inverse Compton (IC) scattering process. Here a shocked wind model with variation of the magnetic parameter $\sigma$ is developed for explaining the observations. By choosing proper param- eters, our model could reproduce two-peak profile in X-ray and TeV light curves. The effect of the disk exhibits an emission and an absorption components in the X-ray and TeV bands respectively. We suggest that some GeV flares will be produced by Doppler boosting the synchrotron spectrum. This model can possibly be used and be checked in other similar systems such as LS I+61o303 and LS 5039.