2024/10/18 by G. Rauw, Rauw, Gregor, R. Blomme +5
Physics and Astronomy · Earth and Planetary Sciences · #Solar and Space Plasma Dynamics #Stellar, planetary, and galactic studies #Geophysics and Gravity Measurements
paper · pdf · doi:10.48550/arxiv.2410.14458
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.