Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...362..318s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 362, Oct. 10, 1990, p. 318-332.
Astronomy and Astrophysics
Astronomy
30
Accretion Disks, Black Holes (Astronomy), Dynamo Theory, Interstellar Magnetic Fields, Kepler Laws, Boundary Conditions, Milky Way Galaxy, Rotating Disks, Steady State
Scientific paper
The combined action of nonuniform rotation and helical convection in protoplanetary disks, in the Galaxy, or in accretion disks surrounding black holes and other compact objects, enables an alpha-omega dynamo to generate a large-scale magnetic field. In this paper, the properties of such magnetic fields are investigated using a two-dimensional, partially numerical method. The structures of the lowest-order steady state and oscillatory modes are calculated for two kinds of external boundary conditions. A quadruple, steady state, highly localized mode is the most easily excited for low values of the dynamo number. The results indicate that, except under special conditions, disk dynamo modes tend to consist of relatively localized rings structures. For large values of the dynamo number, the magnetic field consists of a number of quasi-independent, spatially localized modes generated in various concentric rings filling the disk inward of a dynamo generation 'front'.
Levy Eugene H.
Stepinski Tomasz F.
No associations
LandOfFree
Generation of dynamo magnetic fields in thin Keplerian 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 Generation of dynamo magnetic fields in thin Keplerian disks, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Generation of dynamo magnetic fields in thin Keplerian disks will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1302324