Statistics – Computation
Scientific paper
Dec 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ap%26ss.210...83m&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 210, no. 1-2, p. 83-103 (IAU Colloquium 134)
Statistics
Computation
4
Accretion Disks, Active Galactic Nuclei, Chaos, Thermal Instability, Viscosity, X Ray Binaries, Cataclysmic Variables, Computational Astrophysics, Gas Ionization, Helium, Hydrogen, Protoplanets, Stellar Models
Scientific paper
Basic properties of accretion disk instabilities are summarized. We first explain the standard disk model by Shakura and Sunyaev. In this model, the dominant sources of viscosity are assumed to be chaotic magnetic fields and turbulence in gas flow, and the magnitude of viscosity is prescribed by so-called alpha model. It is then possible to build a particular disk model. In the framework of the standard model, accretion disks are stationary, but when some of the basic assumptions are relaxed, various kinds of instabilities appear. In particular, we focus on the thermal limit-cycle instability caused by partial ionization of hydrogen (and helium). We demonstrate that the disk instability model well accounts for the basic observed features of outbursts of dwarf novae and X-ray nova. We then introduce other kinds of instabilities based on the alpha viscosity model. They are suspected to produce time variabilities observed on a wide range of timescales in close binaries and active galactic nuclei.
No associations
LandOfFree
Accretion disk instabilities 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 Accretion disk instabilities, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Accretion disk instabilities will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-783634