Astronomy and Astrophysics – Astronomy
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.1703b&link_type=abstract
American Astronomical Society Meeting 210, #17.03; Bulletin of the American Astronomical Society, Vol. 39, p.117
Astronomy and Astrophysics
Astronomy
Scientific paper
Earlier in its life our Sun must have rotated considerably more rapidly, given that its magnetized wind slowly carries away angular momentum. Indeed many G-type stars are found to rotate rapidly, and their deep convective envelopes and the dynamos operating there must sense the effects of rotation. Here we use 3-D simulations to study the differential rotation and patterns of convection established in these more rapidly rotating stars. Our simulations with the anelastic spherical harmonic (ASH) code capture the deep solar convection zone with a solar-like radial stratification and within a spherical geometry, which admits global-scale flows. We explore a range of rotation rates from 1 to 10 times the solar rotation rate. Convection in the equatorial regions of these rapidly rotating stars shows strong longitudinal modulation. At the fastest rotation rates, convection is restricted to active nests spanning compact regions in longitude, with quiescent streaming flow filling the regions in between. These nests of convection persist for long periods and drive a strong differential rotation. Convection at high latitudes is more isotropic but couples to the equatorial regions through the meridional circulations present throughout the shell.
Brown Benjamin
Browning Matthew K.
Brun Allan Sacha
Miesch Mark S.
Toomre Juri
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