relation between theta and phi in compton effect

Radio-emitting jets are common in accreting black hole binaries. In the following paper, we present detailed spectra resulting from our equations as applied to Cyg X-1.Īcceleration of particles, radiation mechanisms: non-thermal, binaries: general, radio continuum: stars, X-rays: binaries 1 INTRODUCTION We present a general solution of the kinetic equation with advection and radiative and adiabatic losses and an analytic solution in the case of dominant synchrotron losses in conical jets. Apart from the self-Compton process, we take into account Compton scattering of stellar and accretion photons and absorption of very high energy γ-rays by pair production on soft photons. Our electron kinetic equation includes adiabatic and radiative losses and advection, and our photon radiative transfer equation includes synchrotron absorption and emission and Compton emission. This appears to require a constant dissipation rate per unit logarithmic length and conservation of the magnetic energy flux. Our focus is on the hard spectral state of black hole binaries, for which we take into account that their typical radio spectra are flat. We assume the shape of the rate of electron acceleration and the dependences of its normalization and the magnetic field strength on the height along the jet.

We present here our assumptions, basic equations, and their solutions for the steady-state electron distribution.

This is part one of our study of models of jets with distributed electron acceleration.

Relation between theta and phi in compton effect