Hydrodynamic Turbulence in Accretion Disks
| dc.creator | Mukhopadhyay, Banibrata | |
| dc.creator | Afshordi, Niayesh | |
| dc.creator | Narayan, Ramesh | |
| dc.date | 2005-01-21 | |
| dc.date.accessioned | 2026-07-07T02:16:49Z | |
| dc.date.available | 2026-07-07T02:16:49Z | |
| dc.description | Turbulent viscosity in cold accretion disks is likely to be hydrodynamic in origin. We investigate the growth of hydrodynamic perturbations in a small region of a disk, which we model as a linear shear flow with Coriolis force, between two parallel walls. Although there are no exponentially growing eigenmodes in this system, because of the non-normal nature of the modes, it is possible to have a large transient growth in the energy of certain perturbations. For a constant angular momentum disk, the energy grows by more than a factor of 1000 for a Reynolds number of only 1000, and so turbulence is easily excited. For a Keplerian disk, the growth is more modest, and energy growth by a factor of 1000 requires a Reynolds number of nearly a million. Accretion disks have even larger Reynolds numbers than this. Therefore, transient growth of perturbations could seed turbulence in such disks. | |
| dc.description | 6 pages including 5 figures. To appear in the proceedings of 22nd Texas Symposium on Relativistic Astrophysics, Stanford University, December 13-17, 2004 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0501468 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0501468 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/8936 | |
| dc.subject | Astrophysics | |
| dc.title | Hydrodynamic Turbulence in Accretion Disks | |
| dc.type | text |