Hostname: page-component-7c8c6479df-hgkh8 Total loading time: 0 Render date: 2024-03-28T10:24:15.540Z Has data issue: false hasContentIssue false

Full Sphere Axisymmetric Simulations of the Solar Dynamo

Published online by Cambridge University Press:  14 March 2005

Dibyendu Nandy
Affiliation:
Department of Physics, Montana State University, Bozeman, MT 59717, USA email: nandi@mithra.physics.montana.edu
Piyali Chatterjee
Affiliation:
Department of Physics, Indian Institute of Science, Bangalore 560012, India
Arnab Rai Choudhuri
Affiliation:
Department of Physics, Indian Institute of Science, Bangalore 560012, India
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We explore a full sphere (2D axisymmetric) kinematic solar dynamo model based on the Babcock-Leighton idea that the poloidal field is generated in the surface layers from the decay of tilted bipolar solar active regions. This model incorporates the helioseismically deduced solar rotation profile and an algorithm for buoyancy motivated from simulations of flux tube dynamics. A prescribed deep meridional circulation plays an important role in the advection of magnetic flux. We specifically address the parity issue and show that – contrary to some recent claims – the Babcock-Leighton dynamo can reproduce solar-like dipolar parity if certain reasonable conditions are satisfied in the solar interior, the most important requirement being that the poloidal field of the two hemispheres be efficiently coupled across the equator.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
Contributed Papers
Copyright
© 2004 International Astronomical Union