Astronomy and Astrophysics – Astronomy
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.2414b&link_type=abstract
American Astronomical Society Meeting 210, #24.14; Bulletin of the American Astronomical Society, Vol. 39, p.130
Astronomy and Astrophysics
Astronomy
Scientific paper
Stellar dynamos are powered by the coupling of rotation, convection and the global scale flows which are established in these systems. Our Sun has lost angular momentum through its magnetized wind and once rotated more rapidly than it currently does. We explore the nature of dynamo action in a younger sun rotating five times its current rate. Our explorations employ 3-D simulations of compressible MHD convection within a spherical shell extending from 0.72 to 0.97 solar radii using the anelastic spherical harmonic (ASH) code on massively parallel supercomputers. The dynamo which naturally arises in this convective system is vigorous and builds organized magnetic structures which fill the bulk of the convection zone. This is in striking contrast to the global dynamo thought to operate in the current sun, which appears to require the pumping of magnetic field into a tachocline of shear at the base of the convection zone to generate similar magnetic structures. Particularly in the equatorial regions, we find strong toroidal fields ( 30 kG) coexisting with the turbulent convection. This dynamo system exhibits cyclic behavior, with the large-scale toroidal and poloidal fields switching their polarity.
Brown Benjamin
Brun Allan Sacha
Miesch Mark S.
Toomre Juri
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