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Abstract
Changes in helioseismic mode parameters in active regions and across the solar disk are well documented, but local magnetic activity and geometric effects may not account for all of the scatter seen in the results. We use results from the Helioseismic and Magnetic Imager ring-diagram pipeline for Carrington rotation 2113 to look for differences in mode amplitude and frequency between coronal holes and other quiet-Sun regions. While we do not find a systematic difference, the results do suggest that the correlation between magnetic activity index and mode parameters shows less scatter in coronal hole regions than in general quiet Sun.
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Details
1 School of Physics and Astronomy, University of Birmingham, UK
2 University of Colorado, Boulder, CO, USA
3 Stanford University, USA
4 UCL/MSSL, UK; Department of Physics and Mathematics, University of Hull, UK
5 UCL/MSSL, UK