Speaker
Description
We present a simple semi-analytic model of geometrically-thin accretion flows with significant eccentricity. The structure of the flow, including three-dimensional density profile and velocity field is described by three azimuthally-dependent quantities giving a thickness of the flow in the radial and vertical direction and radial distribution of the angular momentum. These quantities are a set of nonlinear ordinary differential equations. We show that the radial and vertical structure of the flow depart significantly from hydrostatic equilibrium that is commonly assumed in the case of circular flows. We also study oscillations of these flows and find both, the radial and vertical epicyclic modes, at frequencies corresponding to multiples of the flow orbital frequency. Indeed, the amplitude of oscillations change significantly with azimuth; the most of the variability occurs at apocenter.