Differential Rotation and Dynamo Action in Solar-like Stars
S. Brun
CEA Saclay
Main category
Natural Sciences (Physics)
Alternative category
Natural Sciences (Astrophysics and Astrononmy)
The aim of the present study is to characterize the effect of the rotation rate in building magnetic field via dynamo action in solar-like stars. We use the code ASH to model the convective dynamo for solar-like stars at various rotation rates and hence Rossby numbers. We find that stable magnetic configuration without cycling evolution; with steady low latitude magnetic field wreaths are found for slowly rotating cases with large Rossby number. For models rotating faster with a low Rossby number, the convective dynamo shows a cycling activity, leading to systematic pole inversion. We also note that a topology change of the stellar magnetic field occurs going from a dipolar-like to a quadrupolar-like structure when the system magnetic energy drops during the cyclic activity, in good agreement with our star the Sun.
Further information
Further reading
Do you have problems viewing the pdf-file? Download presentation here
If the presentation contains inappropriate content, please report the presentation. You will be redirected to the landing page.