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arXiv · 0907.0069

Probing the Pulsar Wind in the gamma-ray Binary System PSR B1259-63/SS 2883

Jumpei Takata·Ronald E. Taam
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Abstract

The spectral energy distribution from the X-ray to the very high energy regime ($>100$ GeV) has been investigated for the $γ$-ray binary system PSR B1259-63/SS2883 as a function of orbital phase within the framework of a simple model of a pulsar wind nebula. The emission model is based on the synchrotron radiation process for the X-ray regime and the inverse Compton scattering process boosting stellar photons from the Be star companion to the very high energy (100GeV-TeV) regime. With this model, the observed temporal behavior can, in principle, be used to probe the pulsar wind properties at the shock as a function of the orbital phase. Due to theoretical uncertainties in the detailed microphysics of the acceleration process and the conversion of magnetic energy into particle kinetic energy, the observed X-ray data for the entire orbit are fit using two different methods.

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Jumpei Takata, Ronald E. Taam. 2009-07-22. Probing the Pulsar Wind in the gamma-ray Binary System PSR B1259-63/SS 2883. https://doi.org/10.1088/0004-637x%2F702%2F1%2F100

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