Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.4212y&link_type=abstract
American Astronomical Society, HEAD meeting #11, #42.12; Bulletin of the American Astronomical Society, Vol. 41, p.727
Astronomy and Astrophysics
Astronomy
Scientific paper
We present a model of the gamma-ray binary LS 5039 which can explain the spectra and light curves of the TeV, GeV and X-ray observation reasonably well. Assuming that relativistic electrons are injected at a constant rate with a power law spectrum at the location of the compact star, we calculate the gamma-ray production through inverse Compton scattering of soft photons from the companion O star and pair absorption of gamma rays in the same photon field with subsequent cascade processes by the Monte Carlo method. When the power law index of injected electrons is 2.5 with a minimum Lorentz factor of 3x103, GeV to TeV ratio of the resultant flux matches that of the observation data, and the resultant light curves of GeV and TeV emission turns out to anti-correlate. For SUPC, TeV flux takes a minimum due to pair absorption, while GeV flux takes a maximum due to stronger anisotropic Compton scattering. Using the resultant electron number spectrum, we calculate the synchrotron emission assuming constant magnetic field and predict X-ray light curve. X-ray light curve is found to correlate with TeV emission. This is because cooling time of electrons against inverse Compton scattering at INFC is longer than at SUPC and more energy drains into the synchrotron cooling. The amplitude of flux variation in GeV energy band is dependent on the inclination angle and we found that it matches the observation for i=30, while it is larger than the observation for i=60, which suggests that the compact star is a black hole rather than a neutron star. Although qualitative features of the emission spectrum can be reproduced with the present model, the model spectrum does not match the observation in details. We will discuss various possibilities of the extensions of the present simplified model.
Takahara Fumio
Yamaguchi Masaki
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