## 2. Governing equations, initial and boundary conditionsThe set of equations and boundary conditions used here are identical to those in HCb. Further, we use the previous solutions they obtained to initiate the present runs. Using axi-symmetry, HCb solve the radiative hydrodynamical equations consisting of the continuity equation for the density, Euler's equations for three momenta, two equations for the internal energies of the ions and electrons, and one equation for the energy density of the radiation field. In the radiation density equation, HCb modified the opacity
such that the radiation-matter
collisional term reduces to pure
relativistic Bremsstrahlung in
optically thin regions (Stepney & Guilbert 1983) and to the
radiative diffusion operator for higher optical depths. Here
and
denote the density, temperature,
density of radiation and Here, we further include in the ion- and electron-energy equations the corresponding second order conductive operators: where and in cgs units. The subscripts and denote ions and electrons respectively (see & Leer 1994). Gravity of the central object is described in terms of the quasi-newtonian potential of Paczynski & Wiita (1980). A central black hole is assumed and an accretion rate of is set to enter the domain via a thin disk across the outer boundary. The radii in the following are measured in units of In the 2T description (Shapiro et al. 1976), turbulent dissipation heats up the ions only, and subsequently the electrons via Coulomb interaction. For the dynamical viscosity we use as the turbulent diffusion coefficient, where and are used. The calculations are run till the maximum time-independent residual has dropped below a certain small value . This corresponds to several thousand orbital periods of the inner radius.
© European Southern Observatory (ESO) 2000 Online publication: October 30, 2000 |