Non-thermal emission from stellar bow shocks

摘要: Since the detection of non-thermal radio emission from bow shock massive runaway star BD +43$^{\circ}$3654 simple models have predicted high-energy emission, at X and gamma-rays, these Galactic sources. Observational searches for this so far give no conclusive evidence but a few candidates gamma rays. In work we aim developing more sophisticated model shocks. The main goal is to establish whether systems are efficient emitters, even if they not strong enough be yet detected. For modeling collision between stellar wind interstellar medium use 2D hydrodynamic simulations. We then adopt flow profile ambient obtained with simulation as plasma state solving transport energetic particles injected in system, produce. purpose solve 3D (2 spatial + energy) advection-diffusion equation test-particle approximation. find that powerful converts 0.16-0.4% power electrons into mostly produced by inverse Compton scattering dust-emitted photons relativistic electrons, secondly synchrotron radiation. This represents fraction $\sim$ $10^{-5}-10^{-4}$ kinetic power. Given better sensibility current instruments wavelengths theses prone detected through produce rather than energies.