Near-resonant excitation and propagation of eccentric density waves by external forcing

Details Near-resonant excitation and propagation of eccentric density waves by external forcing Near-resonant excitation and propagation of eccentric density waves by external forcing

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...399..192o&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 399, no. 1, p. 192-212.

Statistics

Computation

34

Accretion Disks, Computational Astrophysics, Density Distribution, Star Formation, Wave Excitation, Wave Propagation, Astronomical Models, Companion Stars, Differential Equations, Disturbances, Stellar Orbits, Wentzel-Kramer-Brillouin Method

Scientific paper

An overview is presented of the astronomical evidence that relatively massive, distended, gaseous disks form as a natural by-product of the process of star formation, and also the numerical evidence that SLING-amplified eccentric modes in the outer parts of such disks can drive one-armed spiral density waves in the inner parts by near-resonant excitation and propagation. An ordinary differential equation (ODE) of the second order that approximately governs the nonlocalized forcing of waves in a disk satisfying Lindblad resonance almost everywhere is derived. When transformed and appended with an extra model term, this ODE implies, for free waves, the usual asymptotic results of the WKBJ dispersion relationship and the propagation Goldreich-Tremaine (1978) formula for the resonant torque exerted on a localized Lindblad resonance. An analytical solution is given for the rate of energy and angular momentum transfer by nonlocalized near-resonant forcing in the case when the disk has power-law dependences on the radius of the surface density and temperature.

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