Generation And Dynamics Of Magnetic Fields In The Solar Convection Zone

Details Generation And Dynamics Of Magnetic Fields In The Solar Convection Zone Generation And Dynamics Of Magnetic Fields In The Solar Convection Zone

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e..14n&link_type=abstract

Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech R

Physics

Scientific paper

Magnetic fields constituting solar active regions are generated by a dynamo mechanism in the deep interior of the Sun - from where they buoyantly rise to erupt through the photosphere as sunspots. During this buoyant rise through the convection zone, the magnetic flux tubes interact with a variety of physical processes, notable amongst them being the Coriolis force and helical turbulent convection. This interaction results in the flux tubes acquiring specific structural properties such as tilt and twist. In this talk I will briefly review the process of magnetic field generation and discuss how observations of twist and writhe - components of magnetic helicity - in solar active regions, can constrain the dynamics of magnetic flux tubes in the solar convection zone.

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