Rauw, G. ; Blomme, R. ; Nazé, Y. ; Volpi, D.

published in Bulletin de la Société Royale des Sciences de Liège, 93 issue 3, pp. 256-261 (2024)

Abstract: The O-type long-period binary HD 168112 and triple HD 167971 star systems have been known for several decades for their non-thermal synchrotron radio emission. This emission arises from relativistic electrons accelerated in the hydrodynamic shocks of the wind collisions in these systems. Such wind collisions are expected to produce a strong X-ray emission that varies as a function of orbital phase. In wide eccentric binaries, such as our targets, the X-ray emission arises from an adiabatic plasma and its intensity should scale as the inverse of the orbital separation. We present a set of XMM-Newton observations of these systems which help us gain insight into the properties of their wind interactions.

Keyword(s): stars: early-type ; stars: individual (HD 168112; HD 167971) ; binaries: close ; X-rays: stars
DOI: 10.25518/0037-9565.12337
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