A non-local description of the stress tensor and the accretion disk structure and stability

Details A non-local description of the stress tensor and the accretion disk structure and stability A non-local description of the stress tensor and the accretion disk structure and stability

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasj...46..415k&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 46, no. 4, p. 415-426

Mathematics

Logic

6

Accretion Disks, Acoustic Velocity, Astronomical Models, Oscillations, Pulses, Relativity, Stability, Stress Tensors, Turbulence, Angular Momentum, Approximation, Critical Point, Kinetic Energy, Topology

Scientific paper

In a previous paper we presented an expression for a turbulent stress tensor which does not violate causality. This expression should be applied in cases when the medium has rapid spatial and time variations. In this paper, the expression is applied to studies concerning the structure and stability of a geometrically thin accretion disk. We focus on two problems: (1) the topology and stability of the sonic point of relativistic disks, and (2) the pulsational instability of disks. We find for isothermal disks that the topological type of the sonic point and the stability of the point against small-amplitude perturbations are related: a saddle-type sonic point is stable, while a nodal one is unstable. The possibility that the sonic point is nodal, however, seems to be very low. Second, the new description for the stress tensor acts in a direction so as to dampen the disk oscillations, compared with the case of a local description of the stress tensor. In spite of this, nearly radial local oscillations are still excited in the innermost region of relativistic disks.

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