Journal
ASTRONOMY & ASTROPHYSICS
Volume 449, Issue 2, Pages 451-460Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361:20054241
Keywords
magnetohydrodynamics (MHD); stars : magnetic fields; stars : rotation; stars : evolution; Sun : rotation; instabilities
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We present numerical simulations of a self-sustaining magnetic field in a differentially rotating non-convective stellar interior. A weak initial field is wound up by the differential rotation; the resulting azimuthal field becomes unstable and produces a new meridional field component, which is then wound up anew, thus completing the dynamo loop. This effect is observed both with and without a stable stratification. A self-sustained field is actually obtained more easily in the presence of a stable stratification. The results confirm the analytical expectations of the role of Tayler instability.
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