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Galactic black hole coronae are composed of a hot, magnetized plasma. Thespectral energy distribution produced in this component of X-ray binaries canbe strongly affected by different interactions between locally injectedrelativistic particles and the matter, radiation and magnetic fields in thesource. We study the non-thermal processes driven by the injection ofrelativistic particles into a strongly magnetized corona around an accretingblack hole. We compute in a self-consistent way the effects of relativisticbremsstrahlung, inverse Compton scattering, synchrotron radiation, and thepair-production/annihilation of leptons, as well as hadronic interactions. Ourgoal is to determine the non-thermal broadband radiative output of the corona.The set of coupled kinetic equations for electrons, positrons, protons, andphotons are solved and the resulting particle distributions are computedself-consistently. The spectral energy distributions of transient events inX-ray binaries are calculated, as well as the neutrino production. We show thatthe application to Cygnus X-1 of our model of non-thermal emission from amagnetized corona yields a good fit to the observational data. Finally, we showthat the accumulated signal produced by neutrino bursts in black hole coronaemight be detectable for sources within a few kpc on timescales of years. Ourwork leads to predictions for non-thermal photon and neutrino emissiongenerated around accreting black holes, that can be tested by the newgeneration of very high energy gamma-ray and neutrino instruments.

Particle transport in magnetized media around black holes and associated radiation