UV view of High Mass X-Ray Binary systems (what we know and perspectives for WSO-UV)

Abstract

High Mass X-Ray Binary systems (HMXRB) are composed by a compact object orbiting around a OB massive star. The mass transfer which takes place from the massive star onto its compact companion is the responsible of the emission of high energy photons (X-rays) observed in these systems (to which they owe the name of their class). The presence of a compact object must exert a clear influence in the outer envelopes of the massive star and, thus, must modify the formation and evolution of its stellar wind. Tidal interactions, mass capture and high energy radiation heating and pressure are among the possible ways in which the compact companion and the X-ray emission will influence the stellar wind of the massive counterpart. The status of the observations of such systems from previous UV missions will be reviewed, and perspectives for the incoming WSO-UV space mission will be reported.