Limit cycle instabilities in accretion disks

Details Limit cycle instabilities in accretion disks Limit cycle instabilities in accretion disks

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ans..conf..333m&link_type=abstract

In its Accreting Neutron Stars p 333-337 (SEE N83-15179 05-88)

Statistics

Computation

4

Angular Momentum, Convection, Deposition, Ionization, Radiative Transfer, Star Clusters, Diffusion, Flow Velocity, Irradiation, Stellar Mass, Viscosity, White Dwarf Stars

Scientific paper

Recently, some progress has occurred in the understanding of accretion disk instabilities which are related to a change in the vertical structure of an accretion disk in those parts where partial ionization (mainly of hydrogen) plays a role. In alpha-disks the kinematic viscosity is proportional to the temperature. Therefore together with the latter the inward mass flow velocity caused by viscous diffusion of angular momentum is decreased. In stationary accretion the surface density must then rise in the transition from radiative to convective structure in order to keep the accretion rate constant. Numerical computations show that this rise is so large that the surface density for a convectively structured disk of lower mass accretion rate becomes even larger then that of a radiatively structured disk of higher accretion rate at the same distance from the center. It can easily be shown that stationary accretion then becomes unstable and the disk settles instead into a periodic limit-cycle type of behaviour in which the region in question alternates between a longer phase of cool convective structure with a locally small accretion rate and a shorter phase of hot radiative structure with a locally high mass accretion rate.

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