Resonant excitation of internal gravity waves in cluster cooling flows

Details Resonant excitation of internal gravity waves in cluster cooling flows Resonant excitation of internal gravity waves in cluster cooling flows

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...357..353b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 357, July 10, 1990, p. 353-366.

Astronomy and Astrophysics

Astrophysics

21

Brunt-Vaisala Frequency, Cooling Flows (Astrophysics), Galactic Clusters, Gravity Waves, Internal Waves, Wave Excitation, Energy Dissipation, Gravitational Fields, Resonant Frequencies, Wave Propagation

Scientific paper

Orbital motions of galaxies in X-ray clusters will resonantly excite internal gravity waves (g-waves) that propagate in the plasma. The resonance corresponds to a match between the local Brunt-Vaisala oscillation frequency in the plasma and the appropriate Fourier component of the galactic gravitational potential. Radiated internal waves have an inward group velocity that carries them to the central region of the flow where they become tightly wrapped, geometrically amplified, and eventually dissipated. Waves transport energy and angular momentum, but probably not in amounts large enough to grossly alter the structure of a cooling flow, should one be present. All physical flow variables are finite at the resonance, and all energy and angular momentum deposited by a galaxy is carried inward by the waves. Nonlinear density and velocity fluctuations are likely to result from wave amplitude growth in the central regions of the flow, and a connection with the formation of emission-line filaments is a possibility.

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