Tripathy, S.C. orcid.org/0000-0002-4995-6180, Jain, K. orcid.org/0000-0002-1905-1639, Braun, D. orcid.org/0000-0001-6840-2717 et al. (14 more authors) (2023) Improving the understanding of subsurface structure and dynamics of solar active regions. Bulletin of the American Astronomical Society, 55 (3). ISSN 0002-7537
Abstract
The goal of helioseismology is to provide accurate information about the Sun’s interior from the observations of the wave field at its surface. In the last three decades, both global and local helioseismology studies have made significant advances and breakthroughs in solar physics. However 3-d mapping of the structure and dynamics of sunspots and active regions below the surface has been a challenging task and are among the long standing and intriguing puzzles in solar physics due to the complexity of the turbulent and dynamic nature of magnetized regions. Thus the key problems that need to be addressed during the next decade are: Understanding the wave excitation mechanisms in the quiet Sun and magnetic regions Characterizing the wave propagation and transformation in strong and inclined magnetic field regions and understanding the magnetic portals in the chromosphere Improving helioseismology techniques and investigating the whole life cycle of active regions, from magnetic flux emergence to dissipation Detecting helioseismic signature of the magnetic flux of active regions before it becomes visible on the surface so as to provide warnings several days before the emergence For a transformative progress on these problems require Full disk, simultaneous Doppler and vector magnetic field measurements of the photosphere up to the chromosphere with a spatial resolution of about 2 arc-sec Large-scale radiative MHD simulations of the plasma dynamics from the subphotosphere to the chromosphere Multi-height observations will also able to estimate and correct the center-to-limb variation which is crucial for the measurement of meridional flow in the deeper convection zone including the tachocline region. These measurements will further help to reduce the convective background noise in the power spectra resulting in a more accurate determination of the oscillation frequencies.
Metadata
Item Type: | Article |
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Authors/Creators: |
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Copyright, Publisher and Additional Information: | © 2023 The Authors. This is an Open Access article distributed under the terms of the Creative Commons Attribution Licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. |
Dates: |
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Institution: | The University of Sheffield |
Academic Units: | The University of Sheffield > Faculty of Science (Sheffield) > School of Mathematics and Statistics (Sheffield) |
Depositing User: | Symplectic Sheffield |
Date Deposited: | 18 Oct 2023 14:48 |
Last Modified: | 19 Oct 2023 15:48 |
Status: | Published |
Publisher: | American Astronomical Society |
Refereed: | Yes |
Identification Number: | 10.3847/25c2cfeb.0a945590 |
Open Archives Initiative ID (OAI ID): | oai:eprints.whiterose.ac.uk:204346 |