Abstract
We present our studies of intrabinary shock emission for astrophysical binary systems with a neutron star. We construct a model for the shock emission and compare the model calculation with the light curve and the spectral energy distribution of the gamma-ray binary 1FGL J1018.6-5856. The model assumes a slow and a fast population of particles accelerated in the shock, and computes the high-energy emission spectra and orbital light curves produced by synchrotron, self-Compton and external Compton processes of the high-energy particles in the shock. The model allows one to study plasma properties and to constrain the binary geometry, most importantly the inclination angle (i). We discuss potential use of this model for other pulsar binaries to determine the inclination angle of the binary hence the mass of the neutron star.
Highlights
In some astrophysical binary objects, it is believed that winds of the two objects interact strongly and form shocks, so called intrabinary shocks (IBSs)
We developed an IBS emission model for binary systems in which winds of the two stars interact, producing IBS
We are concerned with high-energy (>Xray) emission in astrophysical binary systems which have a relativistic wind and so can produce a relativistic wind shock
Summary
In some astrophysical binary objects, it is believed that winds of the two objects interact strongly and form shocks, so called intrabinary shocks (IBSs) These shocks can accelerate particles to very high energies, and the particles in the shock radiate high-frequency electromagnetic waves [1]. If one of the stars is a neutron star, the wind of the neutron star is likely composed of cold energetic electrons and positrons When they are accelerated in the shock, they radiate their energy very efficiently. IBS emission can provide us with an independent way of estimating the binary orbital parameters which are important to infer the mass of the neutron star in the binary This can supplement the current method of inferring the neutron star mass with optical spectroscopic and photometric observations and modeling. Note that similar models have been used for other sources such as the gamma-ray binary LS 5039 [8] and the pulsar binary PSR J2215+5135 [9]
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