Modeling the dependence of the X-ray emission of 4U1907 on orbital phase

Details Modeling the dependence of the X-ray emission of 4U1907 on orbital phase Modeling the dependence of the X-ray emission of 4U1907 on orbital phase

Aug 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001icrc....6.2528l&link_type=abstract

Proceedings of the 27th International Cosmic Ray Conference. 07-15 August, 2001. Hamburg, Germany. Under the auspices of the Int

Physics

1

Scientific paper

4U1907+09 is an x-ray binary which has a 437.5 s pulsation period and a 8.38 day orbital period. The mass function is 9 solar masses, implying a B-type or more massive companion to the neutron star. Over an orbital period, 4U1907 exhibits a main peak and a smaller peak in x-ray emission, though both are variable. The neutron star is believed to accrete matter from the stellar wind with the variability due to variations in physical conditions around an eccentric orbit. Long term monitoring of 4U1907 has been done by the RXTE/All-Sky-Monitor. Here, modeling of the 4U1907 system, including the stellar wind, is carried out to explain the x-ray intensity variations with orbital phase.

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