2015/11/12 by Arnab Rai Choudhuri, Gopal Hazra · 1 citation
Biochemistry, Genetics and Molecular Biology · Earth and Planetary Sciences · Physics and Astronomy · #Atmospheric sciences #Buoyancy #Dynamo #Dynamo theory #Flux (metallurgy) #Geomagnetism and Paleomagnetism Studies #Geophysics #Geophysics and Gravity Measurements #Magnetic field #Magnetic flux #Materials science #Mechanics #Physics #Solar and Space Plasma Dynamics #astro-ph.SR
paper · pdf · doi:10.1016/j.asr.2016.03.015
23 pages, 3 figures. Submitted to a special issue of Advances in Space Research on "Solar Dynamo Frontiers"
arxiv created 2015/11/12 · openalex publication_date 2016/03/16 · arxiv updated 2016/09/21 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
One important ingredient of flux transport dynamo models is the rise of the toroidal magnetic field through the convection zone due to magnetic buoyancy to produce bipolar sunspots and then the generation of the poloidal magnetic field from these bipolar sunspots due to the Babcock-Leighton mechanism. Over the years, two methods of treating magnetic buoyancy, a local method and a non-local method have been used widely by different groups in constructing 2D kinematic models of the flux transport dynamo. We review both these methods and conclude that neither of them is fully satisfactory, presumably because magnetic buoyancy is an inherently 3D process. We also point out so far we do not have proper understanding of why sunspot emergence is restricted to rather low latitudes.