Calculations of dynamo coefficients in Parker unstable disks without shear

Details Calculations of dynamo coefficients in Parker unstable disks without shear Calculations of dynamo coefficients in Parker unstable disks without shear

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...408..817o&link_type=abstract

Astronomy and Astrophysics, v.408, p.817-828 (2003)

Astronomy and Astrophysics

Astrophysics

3

Galaxies: Ism, Galaxies: Magnetic Fields, Ism: Magnetic Fields, Mhd

Scientific paper

We investigate the influence of the Coriolis force and magnetic reconnection on the evolution of the Parker instability in galactic disks. We apply a three-dimensional (3D) model of a local gas cube, permeated by an azimuthal regular magnetic field. We numerically solve MHD equations including the contribution of the Coriolis force. At this stage of the investigation we omit the effects of rotational shear. Our previous simulations demonstrate that Parker instability leads to the formation of helically twisted magnetic flux tubes forming a significant poloidal magnetic field component on the scale of the whole cube. Such an evolution represents an example of the fast dynamo process proposed by Parker (\cite{Parker92}). In the present work we extend our earlier computations by calculating the basic coefficients of the MHD dynamo as time-dependent functions. The well-known dynamo coefficients alpha and eta_T - both in the relevant tensorial formulations - are derived from small scale gas motions present in the Parker instability model, so in a local formulation the total turbulent electromotive force (EMF) is described as a quantity dependent on time. The EMF-coefficients alpha and eta_T are evaluated within the limit of high microscopic conductivity.

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