On the possibility of an alpha-sq omega-type dynamo in a thin layer inside the sun

Details On the possibility of an alpha-sq omega-type dynamo in a thin layer inside the sun On the possibility of an alpha-sq omega-type dynamo in a thin layer inside the sun

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...355..733c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 355, June 1, 1990, p. 733-744.

Astronomy and Astrophysics

Astrophysics

53

Dynamo Theory, Solar Interior, Solar Rotation, Magnetic Field Configurations, Solar Magnetic Field, Turbulence Effects

Scientific paper

If the solar dynamo operates in a thin layer of 10,000-km thickness at the interface between the convection zone and the radiative core, using the facts that the dynamo should have a period of 22 years and a half-wavelength of 40 deg in the theta-direction, it is possible to impose restrictions on the values which various dynamo parameters are allowed to have. It is pointed out that the dynamo should be of alpha-sq omega nature, and kinematical calculations are presented for free dynamo waves and for dynamos in thin rectangular slabs with appropriate boundary conditions. An alpha-sq omega dynamo is expected to produce a significant poloidal field which does not leak to the solar surface. It is found that the turbulent diffusity eta and alpha-coefficient are restricted to values within about a factor of 10, the median values being eta of about 10 to the 10th sq cm/sec and alpha of about 10 cm/sec. On the basis of mixing length theory, it is pointed out that such values imply a reasonable turbulent velocity of the order 30 m/s, but rather small turbulent length scales like 300 km.

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