Tidal torques on accretion discs in binary systems with extreme mass ratios.
Abstract
This paper investigates the tidal transport of angular momentum in accretion-disk flow in a close binary system with small mass ratio, q. It is shown that the disk can be tidally truncated only if q is greater than the inverse of the Reynolds number. The existence of a strong 2:1 resonance is derived. Near the resonance, a spiral dissipation pattern is expected. If the Reynolds number is greater than about the inverse square of q, dissipation and angular-momentum loss from the disk may be sufficient to truncate it at the resonance. The application of these results to dwarf novae is discussed.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- March 1979
- DOI:
- 10.1093/mnras/186.4.799
- Bibcode:
- 1979MNRAS.186..799L
- Keywords:
-
- Angular Momentum;
- Binary Stars;
- Momentum Transfer;
- Stellar Mass Accretion;
- Stellar Rotation;
- Transport Properties;
- Disks (Shapes);
- Dwarf Stars;
- Energy Dissipation;
- Light Curve;
- Mass Ratios;
- Novae;
- Reynolds Number;
- Tides;
- Torque;
- Astrophysics;
- Accretion:Dwarf Novae;
- Accretion Disks:Close Binaries