Physics
Scientific paper
Jun 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005kfnts...5..155k&link_type=abstract
Kinematika i Fizika Nebesnykh Tel, Suppl, v. 5, p. 155-158
Physics
Scientific paper
Magnetic buoyancy constrains the magnitude of toroidal field excited by the Ω-effect near the bottom of the solar convection zone (SCZ). Therefore, we examined two negative magnetic buoyancy effects: i) macroscopic turbulent diamagnetism (the γ-effect) and ii) magnetic advection caused by vertical inhomogeneity of plasma density in the SCZ, which we called the nabla ρ-effect. The Sun's rotation which yields the nabla ρ-effect with new properties was taken into account. The reconstruction of toroidal field was calculated as a result of the balance of mean-field magnetic buoyancy, turbulent diamagnetism and the rotationally modified nabla ρ-effect. It is shown that at high latitudes negative buoyancy effects block the magnetic fields in the deep layers of the SCZ, and this may be the most plausible reason why a deep-seated field here could not become as apparent at the solar surface as sunspots. However, in the region located near equator the nabla ρ-effect causes the upward magnetic advection. So, it can facilitate penetration of strong magnetic fields (about 3000-4000 G) to solar surface where they then arise in the ``royal zone'' as the sunspots.
No associations
LandOfFree
Negative magnetic buoyancy and formation of a sunspot belt 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 Negative magnetic buoyancy and formation of a sunspot belt, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Negative magnetic buoyancy and formation of a sunspot belt will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1400279