Other
Scientific paper
May 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...409..360l&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 409, no. 1, p. 360-371.
Other
72
Accretion Disks, Wave Propagation, Cartesian Coordinates, Wentzel-Kramer-Brillouin Method
Scientific paper
We study the propagation properties of 3D oscillating modes in a differentially rotating gaseous disk without self-gravity. We consider mainly axisymmetric waves in a locally vertically isothermal disk and show that the wave structure can be determined analytically. Low-frequency axisymmetric g-modes propagate in a region that lies somewhere inside the wave resonance radius defined by omega = Omega(r), for wave frequency omega and disk angular speed Omega(r). High-frequency axisymmetric p-modes propagate in a region that lies somewhere outside this resonance. Waves exist that cause the disk midplane to oscillate vertically (corrugation waves), as well as waves that keep the disk midplane fixed. For a Keplerian disk, the p-modes and g-modes are separated by a forbidden region for all modes, except for the mode with no vertical nodes (n = 0). Inwardly propagating g-modes become increasingly focused toward the disk midplane, experience a rapidly decreasing radial group velocity, and increasing perturbing velocities near the disk midplane. Such waves can never reach the disk radial center and must almost certainly shock near midplane.
Lubow Stephen H.
Pringle James E.
No associations
LandOfFree
Wave propagation in accretion disks - Axisymmetric case does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Wave propagation in accretion disks - Axisymmetric case, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Wave propagation in accretion disks - Axisymmetric case will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1852776