A model of double coronal hard X-ray sources in solar flares

Kong, Xiangliang; Ye, Jing; Chen, Bin; Guo, Fan; Shen, Chengcai; Li, Xiaocan; Yu, Sijie; Chen, Yao; Giacalone, Joe

doi:10.48550/arxiv.2201.02293

Cited by 2 publications

(3 citation statements)

References 66 publications

(97 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…When particle distributions are nearly isotropic, the Parker transport equation (Parker 1965), where the first-order acceleration is due to flow compression, can describe the time evolution of the distribution function. This equation has recently been adopted in solar flare studies to model particle acceleration in a single large-scale reconnection layer (Li et al 2018b) and flare termination shocks (Kong et al 2019(Kong et al , 2020(Kong et al , 2022. The results show general agreement with certain observed electron spectra and emission signatures in the coronal region.…”

Section: Introductionsupporting

confidence: 59%

See 1 more Smart Citation

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

Guo

Bin

et al. 2022

ApJ

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Section: Introductionsupporting

confidence: 59%

“…Some even larger magnetic islands are ejected upward and collide with the erupted flux rope (y > 70 Mm). Plasma in these regions could be compressed (sometimes a shock may form; see Kong et al 2022), and particles can be accelerated due to compression.…”

Section: Mhd Dynamicsmentioning

confidence: 99%

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

Guo

Bin

et al. 2022

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…When particle distributions are nearly isotropic, the Parker transport equation (Parker 1965), where the first-order acceleration is due to flow compression, can describe the time evolution of the distribution function. This equa-tion has recently been adopted in solar flare studies to model particle acceleration in a single large-scale reconnection layer (Li et al 2018b) and flare termination shocks (Kong et al 2019(Kong et al , 2020(Kong et al , 2022. The results show general agreement with certain observed electron spectra and emission signatures in the coronal region.…”

Section: Introductionsupporting

confidence: 52%

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

Li,

Guo,

Chen

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

The X8.2-class limb flare on September 10, 2017 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.

show abstract

A model of double coronal hard X-ray sources in solar flares

Cited by 2 publications

References 66 publications

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

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

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

Contact Info

Product

Resources

About