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  The Statistical Relationship between White-light Emission and Photospheric Magnetic Field Changes in Flares

Castellanos Durán, J. S., & Kleint, L. (2020). The Statistical Relationship between White-light Emission and Photospheric Magnetic Field Changes in Flares. The Astrophysical Journal, 904(2): 96. doi:10.3847/1538-4357/ab9c1e.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0007-A7F2-B Version Permalink: http://hdl.handle.net/21.11116/0000-0007-A7F3-A
Genre: Journal Article

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 Creators:
Castellanos Durán, Juan Sebastian1, 2, Author              
Kleint, Lucia, Author
Affiliations:
1Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society, Justus-von-Liebig-Weg 3, 37077 Göttingen, DE, ou_1832289              
2IMPRS for Solar System Science at the University of Göttingen, Max Planck Institute for Solar System Research, Max Planck Society, Justus-von-Liebig-Weg 3, 37077 Göttingen, DE, ou_1832290              

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Free keywords: Solar flares ; Solar magnetic fields ; Solar photosphere ; Solar white-light flares
 Abstract: Continuum emission, also called white-light emission (WLE), and permanent changes of the magnetic field (Delta B-LOS) are often observed during solar flares. However, their relation and precise mechanisms are still unknown. We study statistically the relationship between Delta B-LOS and WLE during 75 solar flares of different strengths and locations on the solar disk. We analyze SDO/HMI data and determine for each pixel in each flare if it exhibited WLE and/or Delta B-LOS. We then investigate the occurrence, strength, and spatial size of the WLE, its dependence on flare energy, and its correlation to the occurrence of Delta B-LOS. We detected WLE in 44/75 flares and Delta B-LOS in 59/75 flares. We find that WLE and Delta B-LOS are related, and their locations often overlap between 0% and 60%. Not all locations coincide, thus potentially indicating differences in their origin. We find that the WL area is related to the flare class by a power law, and extend the findings of previous studies, that the WLE is related to the flare class by a power law, to also be valid for C-class flares. To compare unresolved (Sun-as-a-star) WL measurements with our data, we derive a method to calculate temperatures and areas of such data under the blackbody assumption. The calculated unresolved WLE areas improve, but still differ to the resolved flaring area by about a factor of 5-10 (previously 10-20), which could be explained by various physical or instrumental causes. This method could also be applied to stellar flares to determine their temperatures and areas independently.

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Language(s): eng - English
 Dates: 2020
 Publication Status: Published online
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: Peer
 Identifiers: DOI: 10.3847/1538-4357/ab9c1e
 Degree: -

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Title: The Astrophysical Journal
Source Genre: Journal
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Publ. Info: Bristol; Vienna : IOP Publishing; IAEA
Pages: - Volume / Issue: 904 (2) Sequence Number: 96 Start / End Page: - Identifier: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215_3