Probing the Pulsar Wind in the gamma-ray Binary System PSR B1259-63/SS 2883
arXiv:0907.0069 · doi:10.1088/0004-637X/702/1/100
Abstract
The spectral energy distribution from the X-ray to the very high energy regime ( GeV) has been investigated for the -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.
46 pages, 16 figures, accepted for publication in ApJ
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- Periastron Observations of TeV Gamma-Ray Emission from a Binary System with a 50-year Period
- Modelling the light curves of PSR B1259-63/LS 2883-II.The effects of anisotropic pulsar wind and Doppler-boosting
- Modeling high-energy light curves of the PSR B1259-63/LS 2883 binary based on 3-D SPH simulations
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- High-Energy emissions from the Pulsar/Be binary system PSR J2032+4127/MT91 213
- Modeling the multi-wavelength light curves of PSR B1259-63/SS 2883
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- High-energy emissions from the gamma-ray binary LS 5039
- TeV Flux modulation in PSR B1259-63/LS 2883
- Modelling the correlated keV/TeV light curves of Be/gamma-ray binaries
- A new approach to the GeV flare of PSR B1259-63/LS2883
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- Modeling the High-energy Emission from the Gamma-ray Binary 1FGL J1018.6-5856
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