MHD numerical simulations of colliding winds in massive binary systems – I. Thermal versus non-thermal radio emission

摘要: In the past few decades detailed observations of radio and X-ray emission from massive binary systems revealed a whole new physics present in such systems. Both thermal non-thermal components this indicate that most radiation at these bands originates shocks. O B-type stars Wolf–Rayet (WR) supersonic winds that, when colliding, emit largely due to free–free radiation. The emissions are synchrotron inverse Compton processes, respectively. case, magnetic fields expected play an important role distribution. years modelling have been based on purely hydrodynamical simulations, ad hoc assumptions regarding distribution energy field geometry. work we provide first full magnetohydrodynamic numerical simulations wind–wind collision We study characterizing its dependence stellar orbital parameters. also self-consistently evolution shock region, obtaining integrated along different lines sight. show shocks is larger than obtained proportionality between B plasma density assumed. Also, relative total has underestimated.