Statistics – Computation
Scientific paper
Sep 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...332..637a&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 332, Sept. 15, 1988, p. 637-645. Research supported by York University and
Statistics
Computation
23
Accretion Disks, Computational Astrophysics, Galactic Rotation, Gravitational Effects, Viscosity, Many Body Problem, Momentum Transfer, Protoplanets, Quasars
Scientific paper
N-body experiments on an accretion disk comprised of weakly self-gravitating particles in a background Keplerian potential are described. The results show that spiral waves are an important mechanism for the accretion of particles in a rotating disk via angular momentum losses. The spiral waves give a viscosity to the disk that transports angular momentum and causes the particles to spiral slowly toward the central mass. The rate of angular momentum loss is found to be proportional to the fractional disk mass as f exp 7/2. For a 1 percent self-gravitating disk, the time scale for total accretion is found to be on the order of a million rotation periods. An autocorrelation analysis shows that the fundamental potential perturbations are the spiral wakes described by Julian and Toomre (1966). Applications to quasars and protoplanetary disks are briefly discussed.
Anthony D. M.
Carlberg Ray G.
No associations
LandOfFree
Spiral wave viscosity in self-gravitating accretion disks 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 Spiral wave viscosity in self-gravitating accretion disks, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Spiral wave viscosity in self-gravitating accretion disks will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-909462