Accretion disk oscillations - A local analysis in a disk of finite thickness

Details Accretion disk oscillations - A local analysis in a disk of finite thickness Accretion disk oscillations - A local analysis in a disk of finite thickness

Sep 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...296..529c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 296, Sept. 15, 1985, p. 529-539.

Astronomy and Astrophysics

Astrophysics

32

Accretion Disks, Dwarf Novae, Stellar Models, Stellar Oscillations, Gravity Waves, Perturbation, Stability, Two Dimensional Models

Scientific paper

Two types of oscillations are observed to occur in dwarf novae: 'coherent' and 'quasi-periodic' oscillations. These may be associated with the pulsation of the white dwarf or the accretion disk components of the dwarf nova. Here a local (short-wavelength) analysis is utilized to study the oscillation of a self-consistent, two-dimensional model of an accretion disk. The linearized equations describing adiabatic, inviscid, nonaxisymmetric oscillations are used to derive a fifth-order algebraic equation for the (complex) pulsation frequency of the disk. The solutions of this equation for various values of the wavevector k reveal that the disk is capable of supporting (1) a pair of high-frequency acoustic modes (p-modes); (2) a pair of intermediate-frequency modes which may share the characteristics of internal gravity waves (g-modes) and inertial waves; and (3) a mode associated with a dynamical instability (purely imaginary frequency). The role played by the shear in determining the stability or instability of these modes is also considered. Finally, the global oscillation frequencies of the disk are discussed.

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