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Dipolar stability in spherical simulations: The impact of an inner stable zone

Published online by Cambridge University Press:  24 September 2020

Bonnie Zaire Open the ORCID record for Bonnie Zaire [Opens in a new window]  and
Laurène Jouve
Bonnie Zaire
Affiliation:
IRAP, Université de Toulouse, CNRS/UMR 5277, CNES, UPS, 14 avenue E. Belin, Toulouse, F-31400 France email: bzaire@irap.omp.eu
Laurène Jouve
Affiliation:
IRAP, Université de Toulouse, CNRS/UMR 5277, CNES, UPS, 14 avenue E. Belin, Toulouse, F-31400 France email: bzaire@irap.omp.eu
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Abstract

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Magnetic fields vary in complexity for different stars. The stability of dipolar magnetic fields is known to depend on different quantities, e.g., the stellar rotation, the stratification, and the intensity of convective motions. Here, we study the dipolar stability in a system with an inner stable zone. We present preliminary results of dynamo simulations using the Rayleigh number as a control parameter. The stiffness of the stable zone is accordingly varied to keep a constant ratio of the Brunt-Väisälä frequency to the angular velocity. Similarly to the completely convective spherical shell, we find that a transition exists between a regime where the magnetic field is dipolar to a multipolar regime when the Rossby number is increased. The value of the Rossby number at the transition is very close to the one of the fully convective case.

Keywords

Star: magnetic fieldStellar interiors: stably-stratifiedDynamo: simulation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S354: Solar and Stellar Magnetic Fields: Origins and Manifestations , June 2019 , pp. 185 - 188
Copyright
© International Astronomical Union 2020

References

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