A study of the outbursting behavior of the Be X-ray binary, SXP91.1

Be X-ray binaries, which make up the largest subclass of the high mass X-ray binary systems, comprise a neutron star in an eccentric orbit around Be star companion with a geometrically thin Keplerian disc. The interaction of the neutron star with the Be disc results in accretion of matter leading to X-ray outbursts. The X-ray outbursts occur in two flavours: type I and type II. The disc variability is traced through the variability of the emission lines in the optical spectra. In this talk I will present recent results of the outbursting Be X-ray binary, SXP91.1, which is located in the Small Magellanic Cloud. The data from the monitoring campaign of this object was obtained using the optical telescopes, SALT and OGLE, together with X-ray observations from Swift. I will show the analysis performed on these data, where we have studied the variability of the circumstellar disc and how it interacts with the neutron star. Be X-ray binaries, which make up the largest subclass of the high mass X-ray binary systems, comprise a neutron star in an eccentric orbit around Be star companion with a geometrically thin Keplerian disc. The interaction of the neutron star with the Be disc results in accretion of matter leading to X-ray outbursts. The X-ray outbursts occur in two flavours: type I and type II. The disc variability is traced through the variability of the emission lines in the optical spectra. In this talk I will present recent results of the outbursting Be X-ray binary, SXP91.1, which is located in the Small Magellanic Cloud. The data from the monitoring campaign of this object was obtained using the optical telescopes, SALT and OGLE, together with X-ray observations from Swift. I will show the analysis performed on these data, where we have studied the variability of the circumstellar disc and how it interacts with the neutron star.