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Helioseismic insights into the generation and evolution of the Sun’s internal magnetic field

Published online by Cambridge University Press:  24 September 2020

Anne-Marie Broomhall Open the ORCID record for Anne-Marie Broomhall [Opens in a new window]  and
René Kiefer
Anne-Marie Broomhall
Affiliation:
Centre for Fusion, Space and Astrophysics, Department of Physics, University of Warwick, CV4 7AL email: [email protected]
René Kiefer
Affiliation:
Centre for Fusion, Space and Astrophysics, Department of Physics, University of Warwick, CV4 7AL email: [email protected]
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Abstract

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Properties of helioseismic acoustic oscillations (p modes) are modified by flows and magnetic fields in the solar interior, with frequencies, amplitudes and damping rates all varying systematically through the solar cycle. Crucially, now, we have a long enough baseline of helioseismic data to compare of the different activity cycles. We review recent efforts along these lines, from the impact of near-surface magnetic fields on p-mode frequencies to the evolution of the torsional oscillation and meridional circulation. We show that each activity cycle for which we have helioseismic data is slightly different in terms of the relationship between p mode frequencies and atmospheric proxies of activity, and in terms of the rotation and meridional circulation flows. However, many challenges remain, crucially including our ability to constrain flows and magnetic fields in the deep solar interior.

Keywords

Sun: activitySun: helioseismologySun: interiorSun: magnetic fieldsSun: oscillationsSun: rotation
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. 94 - 106
Copyright
© International Astronomical Union 2020

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