The Properties of Compressible MHD and Cosmic Ray Transport
| dc.creator | Lazarian, A. | |
| dc.creator | Cho, Jungyeon | |
| dc.creator | Yan, Huirong | |
| dc.date | 2002-11-02 | |
| dc.date | 2002-11-22 | |
| dc.date.accessioned | 2026-07-07T02:05:58Z | |
| dc.date.available | 2026-07-07T02:05:58Z | |
| dc.description | Turbulence is the most common state of astrophysical flows. In typical astrophysical fluids, turbulence is accompanied by strong magnetic fields, which has a large impact on the dynamics of the turbulent cascade. Recently, there has been a significant breakthrough on the theory of magnetohydrodynamic (MHD) turbulence. For the first time we have a scaling model that is supported by both observations and numerical simulations. We review recent progress in studies of both incompressible and compressible turbulence. We compare Iroshnikov-Kraichnan and Goldreich-Sridhar models, and discuss scalings of Alfven, slow, and fast waves. We discuss the implications of this new insight into MHD turbulence for cosmic ray transport. | |
| dc.description | 27 pages, 7 figures, invited review, to be published in "Recent Reaserch Developments in Astrophyics" (Research Signpost)(slightly modified) | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0211031 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0211031 | |
| dc.identifier | Recent Res. Dev. Astrophys. 1(2003), 297-323 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/5271 | |
| dc.subject | Astrophysics | |
| dc.subject | Fluid Dynamics | |
| dc.subject | Plasma Physics | |
| dc.title | The Properties of Compressible MHD and Cosmic Ray Transport | |
| dc.type | text |