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Photospheric magnetic field variation during solar flares and their implication for the generation of sunquakes

Published online by Cambridge University Press:  28 September 2023

S. Vargas Domínguez Open the ORCID record for S. Vargas Domínguez [Opens in a new window] ,
W. Caicedo Tez  and
J. C. Buitrago Casas
S. Vargas Domínguez
Affiliation:
Universidad Nacional de Colombia, Observatorio Astronómico Nacional
W. Caicedo Tez
Affiliation:
Universidad Nacional de Colombia, Observatorio Astronómico Nacional
J. C. Buitrago Casas
Affiliation:
Space Sciences Laboratory, University of California, Berkeley
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Abstract

Solar flares are an explosive manifestation of the complex magnetic structuring of active regions in the solar atmosphere. The photospheric magnetic field is found to change rapidly, abruptly, and significantly during flaring events. Previous studies are mainly based on line-of-sight or low-cadence data. In this work, we focus on the temporal and spatial evolution of the permanent changes in the magnetic field of solar flares from high-cadence vector data (135 seconds) of the imaging system (dopplergrams and magnetograms) of the SDO/HMI instrument. The highly energetic events under analysis occurred during the solar cycle 24, covering low and high energy ranges, according to GOES classification. This investigation also stands as a crucial input for the characterization and understanding of sunquakes.

Keywords

Sun: activitySun: flaresSun: photosphere
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S372: The Era of Multi-Messenger Solar Physics , August 2022 , pp. 88 - 90
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Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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References

Buitrago-Casas, J. C., et al., 2015, Solar Physics 290.11: 3151–3162.CrossRefGoogle Scholar
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Sharykin, Ivan N., and Kosovichev, Alexander G. ., 2020, ApJ, 895.1: 76. CrossRefGoogle Scholar
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Vargas Domínguez et al. supplementary material

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