Astronomy and Astrophysics – Astronomy
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.1701a&link_type=abstract
American Astronomical Society Meeting 210, #17.01; Bulletin of the American Astronomical Society, Vol. 39, p.117
Astronomy and Astrophysics
Astronomy
Scientific paper
The origin of stellar magnetic fields must rest with dynamo processes occurring deep within a star. Observations of F-type stars suggest unusual relations between their rotation rates and magnetic activity. Generally in cooler stars, magnetic activity increases with more rapid rotation, but, in F-type stars, there is observational evidence for a sharp transition from this behavior around spectral type F5. Stars hotter than F5 show an anti-correlation between magnetic activity and rotation: more rapidly rotating stars seem to possess weaker magnetic fields, possibly because they have less efficient dynamos. We have conducted 3-D simulations of compressible MHD convection with the anelastic spherical harmonic (ASH) code, in order to study F-type star convection zone dynamics in rotating spherical shells. Our initial radial stratification is based on stellar models of stars in the narrow mass range between 1.2 and 1.4 solar masses. We exhibit the resulting differential rotation profiles and rich convective behavior realized as the rotation rates of the stars are increased. We also discuss our preliminary foray into studying the magnetic dynamo achieved within several models, considering the effects of rotation rates.
Augustson Kyle
Brown Benjamin P.
Brun Allan Sacha
Toomre Juri
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