2003/02/01 by В. В. Пипин, V. V. Pipin
Biochemistry, Genetics and Molecular Biology · Physics and Astronomy · #Geomagnetism and Paleomagnetism Studies #Solar and Space Plasma Dynamics #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1080/0309192021000053366
published as GAFD, 2003, v.97,pp.25-43 · 20 pages, 6 figures
openalex publication_date 2003/02/01 · arxiv created 2005/03/04 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/29
We explore the f -effect and the small-scale current helicity, , for the case of weakly compressible magnetically driven turbulence that is subjected to the differential rotation. No restriction is applied to the amplitude of angular velocity, i.e., the derivations presented are valid for an arbitrary Coriolis number, z * = 2 z cor , though the differential rotation itself is assumed to be weak. The expressions obtained are used to explore the possible distributions of f -effect and h c in convection zones (CZ) of the solar-type stars. Generally, our theory gives f > 0 in the northern hemisphere of the Sun and the opposite case in the southern hemisphere. In most cases the h c has the opposite sign to f . However, we show that in the depth of CZ where the influence of rotation upon turbulence (associated with z *) and the radial shear of angular velocity are strong, the distribution of f might be drastically different from a classical cos è -dependence, where è is colatitude. It is shown that f has a negative sign at the bottom and below of CZ at mid latitudes. There, the distribution of h c is also different from cos è , but it does not change its sign with the depth. Further, we briefly consider these quantities in the disk geometry. The application of the developed theory to dynamos in the accretion disk is more restrictive because they usually have a strong differential rotation, | ‘ log z / ‘ log r | > 1.