Physics
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.0407b&link_type=abstract
American Astronomical Society, SPD meeting #40, #4.07; Bulletin of the American Astronomical Society, Vol. 41, p.811
Physics
Scientific paper
When stars like our Sun are young, they rotate much more rapidly than the Sun currently does. Young, rapidly rotating suns also appear to have substantial magnetic activity and perhaps strong axisymmetric magnetic fields. We explore the complex coupling between rotation, convection and magnetism in rapidly rotating suns with 3-D MHD simulations using the anelastic spherical harmonic (ASH) code. We find that substantial organized global-scale magnetic fields are realized by dynamo action in these systems. In the bulk of the convection zone, global-scale wreathes of magnetism arise and coexist with the strongly turbulent convection. This is a great surprise, as these simulations do not include tachoclines of shear and penetration. The tachocline is a crucial ingredient in many solar dynamo theories, and to date, global simulations of the solar dynamo have required a tachocline to achieve global-scale organization of magnetic field. Here we will explore how such wreathes might be built in rapidly rotating suns, how they are maintained in the midst of the convection zone, and how they undergo cycles of activity, where the fields wax and wane in strength and can even change in global 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), Nicholas J. Nelson and Juri Toomre (both University of Colorado, Boulder).
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