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The Suppression and Promotion of Magnetic Flux Emergence in Fully Convective Stars

Published online by Cambridge University Press:  12 September 2017

Maria A. Weber ,
Matthew K. Browning ,
Suzannah Boardman ,
Joshua Clarke ,
Samuel Pugsley  and
Edward Townsend
Maria A. Weber
Affiliation:
Department of Physics and Astronomy, University of Exeter, Stocker Road, EX4 4QL Exeter, UK email: mweber@astro.ex.ac.uk
Matthew K. Browning
Affiliation:
Department of Physics and Astronomy, University of Exeter, Stocker Road, EX4 4QL Exeter, UK email: mweber@astro.ex.ac.uk
Suzannah Boardman
Affiliation:
Department of Physics and Astronomy, University of Exeter, Stocker Road, EX4 4QL Exeter, UK email: mweber@astro.ex.ac.uk
Joshua Clarke
Affiliation:
Department of Physics and Astronomy, University of Exeter, Stocker Road, EX4 4QL Exeter, UK email: mweber@astro.ex.ac.uk
Samuel Pugsley
Affiliation:
Department of Physics and Astronomy, University of Exeter, Stocker Road, EX4 4QL Exeter, UK email: mweber@astro.ex.ac.uk
Edward Townsend
Affiliation:
Department of Physics and Astronomy, University of Exeter, Stocker Road, EX4 4QL Exeter, UK email: mweber@astro.ex.ac.uk
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Abstract

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Evidence of surface magnetism is now observed on an increasing number of cool stars. The detailed manner by which dynamo-generated magnetic fields giving rise to starspots traverse the convection zone still remains unclear. Some insight into this flux emergence mechanism has been gained by assuming bundles of magnetic field can be represented by idealized thin flux tubes (TFTs). Weber & Browning (2016) have recently investigated how individual flux tubes might evolve in a 0.3M⊙ M dwarf by effectively embedding TFTs in time-dependent flows representative of a fully convective star. We expand upon this work by initiating flux tubes at various depths in the upper ~50-75% of the star in order to sample the differing convective flow pattern and differential rotation across this region. Specifically, we comment on the role of differential rotation and time-varying flows in both the suppression and promotion of the magnetic flux emergence process.

Keywords

MHDstars: magnetic fieldsstars: spotsstars: interiorsmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S328: Living Around Active Stars , October 2016 , pp. 85 - 92
Copyright
Copyright © International Astronomical Union 2017 

References

Abbett, W. P., Fisher, G. H., Fan, Y., & Bercik, D. J., 2004, ApJ, 612, 557 Google Scholar
Browning, M. K., 2008, ApJ, 676, 1262 Google Scholar
Charbonneau, P., 2010, Living Reviews in Solar Physics, 7, 3 CrossRefGoogle Scholar
Clyne, J., Mininni, P., Norton, A., & Rast, M., 2007, New Journal of Physics, 9, 301 Google Scholar
Dobler, W., Stix, M., & Brandenburg, A., 2006, ApJ, 638, 336 Google Scholar
Fan, Y., 2009, Living Reviews in Solar Physics, 6, 4 Google Scholar
Nelson, N. J., Brown, B. P., Brun, A. S., Miesch, M. S., & Toomre, J., 2011, ApJL, 739, L38 Google Scholar
Roberts, B. & Webb, A. R., 1978, SoPh, 56, 5 Google Scholar
Spruit, H. C., 1981, A&A, 98, 155 Google Scholar
Tobias, S. M., Brummell, N. H., Clune, T. L., & Toomre, J., 2001, ApJ, 549, 1183 Google Scholar
Weber, M. A. & Browning, M. K., 2016, ApJ, 827, 95 Google Scholar
Weber, M. A., Fan, Y., & Miesch, M. S., 2013, SoPh, 287, 239 Google Scholar
West, A. A., Weisenburger, K. L., Irwin, J., et al., 2015, ApJ, 812, 3 Google Scholar
Wright, N. J. & Drake, J. J., 2016, Nature, 535, 526 Google Scholar
Yadav, R. K., Christensen, U. R., Morin, J., et al., 2015, ApJL, 813, L31 Google Scholar
Zwaan, C., 1987, ARA&A, 25, 83 Google Scholar