Modeling Electron Acceleration and Transport in the Early Impulsive Phase of the 2017 September 10th Solar Flare

Xiaocan Li; Fan Guo; Bin Chen; Chengcai Shen; Lindsay Glesener

doi:10.3847/1538-4357/ac6efe

Modeling Electron Acceleration and Transport in the Early Impulsive Phase of the 2017 September 10th Solar Flare

Xiaocan Li
, Fan Guo
, Bin Chen
, Chengcai Shen
, Lindsay Glesener

Physics and Astronomy (Twin Cities)

Research output: Contribution to journal › Article › peer-review

27 Scopus citations

Abstract

The X8.2-class limb flare on 2017 September 10 is among the best studied solar flare events owing to its great similarity to the standard flare model and the broad coverage by multiple spacecraft and ground-based observations. These multiwavelength observations indicate that electron acceleration and transport are efficient in the reconnection and flare looptop regions. However, there lacks a comprehensive model for explaining and interpreting the multi-faceted observations. In this work, we model the electron acceleration and transport in the early impulsive phase of this flare. We solve the Parker transport equation that includes the primary acceleration mechanism during magnetic reconnection in the large-scale flare region modeled by MHD simulations. We find that electrons are accelerated up to several MeV and fill a large volume of the reconnection region, similar to the observations shown in microwaves. The electron spatial distribution and spectral shape in the looptop region agree well with those derived from the microwave and hard X-ray emissions before magnetic islands grow large and dominate the acceleration. Future emission modelings using the electron maps will enable direct comparison with microwave and hard X-ray observations. These results shed new light on the electron acceleration and transport in a broad region of solar flares within a data-constrained realistic flare geometry.

Original language	English (US)
Article number	92
Journal	Astrophysical Journal
Volume	932
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/ac6efe
State	Published - Jun 1 2022

Bibliographical note

Funding Information:
We thank the anonymous referee for very helpful and constructive review. X.L. acknowledges the support from NASA through grant No. 80NSSC21K1313, National Science Foundation grant No. AST-2107745, and Los Alamos National Laboratory through subcontract No. 622828. F.G. acknowledges the support from NASA grant Nos. 80HQTR20T0073, 80HQTR20T0040, 80HQTR21T0087, and 80HQTR21T0103, NSF grant No. AST-2109154, and the support of the LDRD program at LANL. B.C. acknowledges the support from NASA grant No. 80NSSC20K1318 and NSF grant Nos. AGS-1654382 and AST-2108853 to NJIT. C.S. acknowledges the support from NASA through grant No. 80NSSC21K2044 and National Science Foundation grant No. AST-2108438. Simulations were performed at the National Energy Research Scientific Computing Center (NERSC) and the Texas Advanced Computing Center (TACC) at The University of Texas at Austin. This work was facilitated in part by the NASA Drive Science Center on Solar Flare Energy Release (SolFER).

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© 2022. The Author(s). Published by the American Astronomical Society.

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title = "Modeling Electron Acceleration and Transport in the Early Impulsive Phase of the 2017 September 10th Solar Flare",

abstract = "The X8.2-class limb flare on 2017 September 10 is among the best studied solar flare events owing to its great similarity to the standard flare model and the broad coverage by multiple spacecraft and ground-based observations. These multiwavelength observations indicate that electron acceleration and transport are efficient in the reconnection and flare looptop regions. However, there lacks a comprehensive model for explaining and interpreting the multi-faceted observations. In this work, we model the electron acceleration and transport in the early impulsive phase of this flare. We solve the Parker transport equation that includes the primary acceleration mechanism during magnetic reconnection in the large-scale flare region modeled by MHD simulations. We find that electrons are accelerated up to several MeV and fill a large volume of the reconnection region, similar to the observations shown in microwaves. The electron spatial distribution and spectral shape in the looptop region agree well with those derived from the microwave and hard X-ray emissions before magnetic islands grow large and dominate the acceleration. Future emission modelings using the electron maps will enable direct comparison with microwave and hard X-ray observations. These results shed new light on the electron acceleration and transport in a broad region of solar flares within a data-constrained realistic flare geometry.",

author = "Xiaocan Li and Fan Guo and Bin Chen and Chengcai Shen and Lindsay Glesener",

note = "Funding Information: We thank the anonymous referee for very helpful and constructive review. X.L. acknowledges the support from NASA through grant No. 80NSSC21K1313, National Science Foundation grant No. AST-2107745, and Los Alamos National Laboratory through subcontract No. 622828. F.G. acknowledges the support from NASA grant Nos. 80HQTR20T0073, 80HQTR20T0040, 80HQTR21T0087, and 80HQTR21T0103, NSF grant No. AST-2109154, and the support of the LDRD program at LANL. B.C. acknowledges the support from NASA grant No. 80NSSC20K1318 and NSF grant Nos. AGS-1654382 and AST-2108853 to NJIT. C.S. acknowledges the support from NASA through grant No. 80NSSC21K2044 and National Science Foundation grant No. AST-2108438. Simulations were performed at the National Energy Research Scientific Computing Center (NERSC) and the Texas Advanced Computing Center (TACC) at The University of Texas at Austin. This work was facilitated in part by the NASA Drive Science Center on Solar Flare Energy Release (SolFER). Publisher Copyright: {\textcopyright} 2022. The Author(s). Published by the American Astronomical Society.",

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doi = "10.3847/1538-4357/ac6efe",

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AU - Shen, Chengcai

AU - Glesener, Lindsay

N1 - Funding Information: We thank the anonymous referee for very helpful and constructive review. X.L. acknowledges the support from NASA through grant No. 80NSSC21K1313, National Science Foundation grant No. AST-2107745, and Los Alamos National Laboratory through subcontract No. 622828. F.G. acknowledges the support from NASA grant Nos. 80HQTR20T0073, 80HQTR20T0040, 80HQTR21T0087, and 80HQTR21T0103, NSF grant No. AST-2109154, and the support of the LDRD program at LANL. B.C. acknowledges the support from NASA grant No. 80NSSC20K1318 and NSF grant Nos. AGS-1654382 and AST-2108853 to NJIT. C.S. acknowledges the support from NASA through grant No. 80NSSC21K2044 and National Science Foundation grant No. AST-2108438. Simulations were performed at the National Energy Research Scientific Computing Center (NERSC) and the Texas Advanced Computing Center (TACC) at The University of Texas at Austin. This work was facilitated in part by the NASA Drive Science Center on Solar Flare Energy Release (SolFER). Publisher Copyright: © 2022. The Author(s). Published by the American Astronomical Society.

PY - 2022/6/1

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N2 - The X8.2-class limb flare on 2017 September 10 is among the best studied solar flare events owing to its great similarity to the standard flare model and the broad coverage by multiple spacecraft and ground-based observations. These multiwavelength observations indicate that electron acceleration and transport are efficient in the reconnection and flare looptop regions. However, there lacks a comprehensive model for explaining and interpreting the multi-faceted observations. In this work, we model the electron acceleration and transport in the early impulsive phase of this flare. We solve the Parker transport equation that includes the primary acceleration mechanism during magnetic reconnection in the large-scale flare region modeled by MHD simulations. We find that electrons are accelerated up to several MeV and fill a large volume of the reconnection region, similar to the observations shown in microwaves. The electron spatial distribution and spectral shape in the looptop region agree well with those derived from the microwave and hard X-ray emissions before magnetic islands grow large and dominate the acceleration. Future emission modelings using the electron maps will enable direct comparison with microwave and hard X-ray observations. These results shed new light on the electron acceleration and transport in a broad region of solar flares within a data-constrained realistic flare geometry.

AB - The X8.2-class limb flare on 2017 September 10 is among the best studied solar flare events owing to its great similarity to the standard flare model and the broad coverage by multiple spacecraft and ground-based observations. These multiwavelength observations indicate that electron acceleration and transport are efficient in the reconnection and flare looptop regions. However, there lacks a comprehensive model for explaining and interpreting the multi-faceted observations. In this work, we model the electron acceleration and transport in the early impulsive phase of this flare. We solve the Parker transport equation that includes the primary acceleration mechanism during magnetic reconnection in the large-scale flare region modeled by MHD simulations. We find that electrons are accelerated up to several MeV and fill a large volume of the reconnection region, similar to the observations shown in microwaves. The electron spatial distribution and spectral shape in the looptop region agree well with those derived from the microwave and hard X-ray emissions before magnetic islands grow large and dominate the acceleration. Future emission modelings using the electron maps will enable direct comparison with microwave and hard X-ray observations. These results shed new light on the electron acceleration and transport in a broad region of solar flares within a data-constrained realistic flare geometry.

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JO - Astrophysical Journal

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ER -

Modeling Electron Acceleration and Transport in the Early Impulsive Phase of the 2017 September 10th Solar Flare

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