Modeling the non-thermal emission from bowshocks produced by runaway stars

Runaway O- and early B-type stars passing throughout the interstellar medium at supersonic velocities and characterized by strong stellar winds, can produce bow shocks that can serve as particle acceleration sites. Previous theoretical models predict the production of high energy photons by non-thermal radiative processes, but their efficiency is still debated. We present a new insight in the non-thermal emission treatment by introducing new approaches, new formulae and exploring the computational method to search for sistematic errors, and we also test its feasibility. We applied our model to AE Aurigae, the first reported star with an X-ray detected bow shock (López-Santiago et al. 2012), and BD+43º3654, in which the observations failed in detecting high-energy emission. From our analysis, we confirm that the X-ray emission from the bow shock produced by AE Aurigae can be explained by inverse Compton processes involving the infrared photons of the heated dust. We also predict low high-energy flux emission from the bow shock produced by BD+43º3654, which explains its non detection in X-rays by Terada et al. (2012).