Models and theoretical spectra of accretion discs in dwarf novae.
Abstract
Attention is given to a new technique for modelling dwarf novae accretion disks which permits the consistent determination of disk structure together with the radiation field. A cylindrically symmetric disk is divided into a set of concentric rings, each of them behaving independently, like a plane-parallel radiating slab. The vertical structure of each ring is determined by the joint solution of hydrostatic equilibrium, energy balance and radiative transfer equations. Numerical computations were carried out for a stationary disk with a central star having a mass equal to 1 solar mass and a radius equal to 5 x 10 to the 8th cm; the mass flux through the disk is taken to be 10 to the -8th, 10 to the -10th, and 10 to the -11th the solar mass per yr. Comparison of the theoretical radiative flux distribution with the observed distribution of the white dwarf WX Hyi reveals that the quiescent state of Wx Hyi corresponds to a mass flux of about 10 to the -11th the solar mass per yr.
- Publication:
-
Bulletin of the Astronomical Institutes of Czechoslovakia
- Pub Date:
- May 1986
- Bibcode:
- 1986BAICz..37..129K
- Keywords:
-
- Accretion Disks;
- Dwarf Novae;
- Stellar Models;
- Stellar Radiation;
- Stellar Spectra;
- White Dwarf Stars;
- Computational Astrophysics;
- Equilibrium Equations;
- Radiative Transfer;
- Stellar Atmospheres;
- Astrophysics