Can we detect local helioseismic parameter shifts in coronal holes?

Howe, R; Haber, D A; Bogart, R S; Zharkov, S; Baker, D; Harra, L; Driel-Gesztelyi, L. Van

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 theHelioseismic and Magnetic Imagerring-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.

Citation

Howe, R., Haber, D. A., Bogart, R. S., Zharkov, S., Baker, D., Harra, L., & Driel-Gesztelyi, L. V. (2013). Can we detect local helioseismic parameter shifts in coronal holes?. Journal of Physics: Conference Series, 440(1), 012019. https://doi.org/10.1088/1742-6596/440/1/012019

• Journal Article Type: Conference Paper
• Acceptance Date: Jun 1, 2013
• Online Publication Date: Jun 11, 2013
• Publication Date: Jun 11, 2013
• Deposit Date: Aug 2, 2018
• Publicly Available Date: Aug 3, 2018
• Print ISSN: 1742-6588
• Electronic ISSN: 1742-6596
• Publisher: IOP Publishing
• Peer Reviewed: Peer Reviewed
• Volume: 440
• Issue: 1
• Article Number: 012019
• Pages: 012019
• DOI: https://doi.org/10.1088/1742-6596/440/1/012019
• Public URL: https://hull-repository.worktribe.com/output/429205
• Publisher URL: http://iopscience.iop.org/article/10.1088/1742-6596/440/1/012019/meta