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

Arnab Rai, Choudhuri (1990) On the possibility of an alpha-sq omega-type dynamo in a thin layer inside the sun Astrophysical Journal, 355 . pp. 733-744. ISSN 0004-637X

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Official URL: http://adsabs.harvard.edu/doi/10.1086/168806

Related URL: http://dx.doi.org/10.1086/168806


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.

Item Type:Article
Source:Copyright of this article belongs to The American Astronomical Society.
Keywords:Dynamo theory; Solar interior; Solar rotation; Magnetic field configurations; Solar magnetic field; Turbulence effects
ID Code:66566
Deposited On:25 Jun 2012 13:34
Last Modified:25 Jun 2012 13:34

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