Exploring stream accretion in high mass X-ray binaries

This work focuses on the method of accretion in supergiant X-ray binary systems. Analysis of twelve years of observations from the Rossi X-ray Timing Explorer All-Sky Monitor folded at the orbital period is carried out for the following systems: 4U 1907+09, GX 301-2, OAO 1657-415 and 2S 0114+650. Each orbital X-ray light curve is compared to the expected light curve of a system with the mechanism of accretion being a stream originating at the surface of the companion star along with strong stellar winds. Orbital parameters of each system are taken as inputs for the wind and stream accretion model and statistical analysis is done to constrain the properties of the stellar wind and gas stream. We find that the systems 4U 1907+09 and GX 301-2 likely contain a dynamic gas stream that significantly contributes to the production of X-ray radiation. Further analysis is required to accurately determine the accretion mechanism in OAO 1657-415; preliminary results point to the possibility of stream accretion. The binary system 2S 0114+650 appears to be undergoing accretion via stellar wind capture.