Ponente
Descripción
Gamma-ray binaries produce the majority of their multi-wavelength non-thermal emission at energies >1 MeV. These systems consist of an O/Be star and a compact object, which has been detected as a neutron star in 3 of the 9 systems. It is largely understood, then, that the VHE non-thermal emission in these systems originates in a stand-off shock that is produced when the stellar wind and/or disc of the O/Be companion collides with the relativistic pulsar wind from the young neutron star.
The Be gamma-ray binary HESS J0632+057 has a ~317.3 d orbital period and displays a double-peaked profile in both the X-ray and TeV lightcurves, which is believed to be due to the pulsar crossing/interacting with the circumstellar disc, similar to what is observed in the other Be gamma-ray binary systems. We report on the new orbital solution for this system, obtained from optical spectroscopic data obtained with SALT which will allow for a simpler interpretation of the two peaks in the non-thermal emission. Furthermore, we investigate the impact of the disc on the optical as well as high energy emission with the implementation of a toy-model of the circumstellar disc in these systems.
