Global-Scale Stellar Dynamos and Wreathes of Magnetism in Rapidly Rotating Suns Without Tachoclines

Details Global-Scale Stellar Dynamos and Wreathes of Magnetism in Rapidly Rotating Suns Without Tachoclines Global-Scale Stellar Dynamos and Wreathes of Magnetism in Rapidly Rotating Suns Without Tachoclines

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21331406b&link_type=abstract

American Astronomical Society, AAS Meeting #213, #314.06; Bulletin of the American Astronomical Society, Vol. 41, p.292

Physics

Scientific paper

When our sun was young it rotated much more rapidly than it currently does. Observations of young, rapidly rotating stars indicate that they possess substantial magnetic activity and strong axisymmetric magnetic fields. We conduct simulations of dynamo action in more rapidly rotating suns with the 3-D MHD anelastic spherical harmonic (ASH) code to explore the complex coupling between rotation, convection and magnetism. We find that substantial organized global-scale magnetic fields are achieved by dynamo action in these systems. Wreathes of magnetism are built in the midst of the convection zone, coexisting with the intensely turbulent convection. This is a great surprise, as many solar dynamo theories have indicated that a tachocline of penetration and shear at the base of the convection zone is a crucial ingredient for organized dynamo action, whereas these simulations do not include such tachoclines. The dynamos achieved in these rapidly rotating stars can undergo cycles of activity, with fields waxing and waning in strength and even changing polarity. This research was carried out with support by the NASA HelioPhysics Theory program and with additional support for Brown by the NASA GSRP program. This thesis research has been done in collaboration with Matthew K. Browning (CITA, Toronto), Allan Sacha Brun (CEA-Saclay, France), Mark S. Miesch (HAO, Boulder) and Juri Toomre (University of Colorado, Boulder).

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