Stability, Instability, and "Backwards'' Transport in Accretion Disks"

Details Stability, Instability, and "Backwards'' Transport in Accretion Disks" Stability, Instability, and "Backwards'' Transport in Accretion Disks"

1999-06-18

arxiv.org/abs/astro-ph/9906315v2

Astronomy and Astrophysics

Astrophysics

21 pages, 5 figs., AAS LaTEX macros v4.0. Accepted to ApJ, final version

Scientific paper

10.1086/308732

The stratification of entropy and the stratification of angular momentum are closely analogous. Of particular interest is the behavior of disks in which angular momentum transport is controlled by convection, and heat transport by dynamical turbulence. In both instances we argue that the transport must proceed ``backwards'' relative to the sense one would expect from a simple enhanced diffusion approach. Reversed angular momentum transport has already been seen in numerical simulations; contra-gradient thermal diffusion should be amenable to numerical verification as well. These arguments also bear on the observed nonlinear local stability of isolated Keplerian disks. We also describe a diffusive instability that is the entropy analogue to the magnetorotational instability. It affects thermally stratified layers when Coulomb conduction and a weak magnetic field are present. The criterion for convective instability goes from one of upwardly decreasing entropy to one of upwardly decreasing temperature. The maximum growth rate is of order the inverse sound crossing time, independent of the thermal conductivity. The indifference of the growth rate to the conduction coefficient, its simple dynamical scaling, and the replacement in the stability criterion of a conserved quantity (entropy) gradient by a free energy (temperature) gradient are properties similar to those exhibited by the magnetorotational instability.

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