Numerical models of 3-D galactic dynamos

Details Numerical models of 3-D galactic dynamos Numerical models of 3-D galactic dynamos

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...264...77p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 264, no. 1, p. 77-85.

Astronomy and Astrophysics

Astrophysics

13

Dynamo Theory, Galactic Structure, Mathematical Models, Three Dimensional Models, Computerized Simulation, Field Strength, Interstellar Magnetic Fields, Shock Waves, Turbulence Effects

Scientific paper

We describe here the results of 3-d numerical simulations of an Alpha-omega dynamo in galaxies with differential rotation, small scale turbulence, and a shock wave induced by a stellar density wave. A non-linear quenching mechanism for the dynamo instability is used, and with the model parameters employed the field achieves a steady-state which closely resembles observed fields in galaxies. The magnetic field vectors are parallel to the plane in the disk, with the magnetic intensity decreasing away from the plane. The vectors are also nearly parallel to the spiral arms in the disk, and the field direction is axisymmetric about the galactic center, but with significant increase of intensity in the arms. The magnetic intensity rises steeply towards the center of the galaxy, where the field becomes dominated by the vertical component. Nowhere in the parameter range covered is the bisymmetric field mode dominant.

Affiliated with

Also associated with

No associations

Rating

Numerical models of 3-D galactic dynamos 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 Numerical models of 3-D galactic dynamos, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Numerical models of 3-D galactic dynamos will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1868086