First Report of a Solar Energetic Particle Event Observed by China’s Tianwen-1 Mission in Transit to Mars

Fu, Shuai; Ding, Zheyi; Zhang, Yongjie; Zhang, Xiaoping; Li, Cunhui; Li, Gang; Tang, S.W.; Zhang, Haiyan; Xu, Yi; Wang, Yuming; Guo, Jingnan; Zhao, Lingling; Wang, Yi; Hu, Xiangyu; Luo, P. W.; Sun, Z.; Yu, Yuhong; Xie, Luhua

doi:10.3847/2041-8213/ac80f5

Cited by 6 publications

(2 citation statements)

References 56 publications

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“…Besides the wide spreading of SEPs, other interesting characteristics of this SEP event have been discussed, such as the significant depletion of SEPs associated with the interaction between the shock and a magnetic structure by Giacalone et al (2021), the similarity and differences of ion spectra at four spacecraft by Mason et al (2021), and the observation of inverted energy spectra due to the passage of previous CME (Lario et al 2021). More recently, the observation of this event near Mars as observed by Tianwen-1 was reported by Fu et al (2022). Despite the fact that many observational studies have been devoted to this event, a range of comprehensive modeling efforts on this SEP event are still lacking.…”

Section: Introductionmentioning

confidence: 83%

Modeling the 2020 November 29 solar energetic particle event using EUHFORIA and iPATH models

Ding

Wijsen

et al. 2022

A&A

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Aims. We present the implementation of a coupling between EUropean Heliospheric FORcasting Information Asset (EUHFORIA) and improved Particle Acceleration and Transport in the Heliosphere (iPATH) models. In this work, we simulate the widespread solar energetic particle (SEP) event of 2020 November 29 and compare the simulated time-intensity profiles with measurements at Parker Solar Probe (PSP), the Solar Terrestrial Relations Observatory (STEREO)-A, SOlar and Heliospheric Observatory (SOHO), and Solar Orbiter (SolO). We focus on the influence of the history of shock acceleration on the varying SEP time-intensity profiles and investigate the underlying causes in the origin of this widespread SEP event.Methods. We simulated a magnetized coronal mass ejection (CME) propagating in the data-driven solar wind with the EUHFORIA code. The CME was initiated by using the linear force-free spheromak module of EUHFORIA. The shock parameters and a 3D shell structure were computed from EUHFORIA as inputs for the iPATH model. Within the iPATH model, the steady-state solution of particle distribution assuming diffuse shock acceleration is obtained at the shock front. The subsequent SEP transport is described by the focused transport equation using the backward stochastic differential equation method with perpendicular diffusion included. Results. We examined the temporal evolution of shock parameters and particle fluxes during this event and we find that adopting a realistic solar wind background can significantly impact the expansion of the shock and, consequently, the shock parameters. Timeintensity profiles with an energetic storm particle event at PSP are well reproduced from the simulations. In addition, the simulated and observed time-intensity profiles of protons show a similar two-phase enhancement at STA. These results illustrate that modeling a shock using a realistic solar wind is crucial in determining the characteristics of SEP events. The decay phase of the modeled time-intensity profiles at Earth is in good agreement with the observations, indicating the importance of perpendicular diffusion in widespread SEP events. Taking into account the possible large curved magnetic field line connecting to SolO, the modeled timeintensity profiles show a good agreement with the observation. We suggest that the broadly distorted magnetic field lines, which are due to a stream interaction region, may be a key factor in helping to improve our understanding of the observed SEPs at SolO for this event.

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Section: Introductionmentioning

confidence: 83%

Modeling the 2020 November 29 solar energetic particle event using EUHFORIA and iPATH models

Ding

Wijsen

et al. 2022

A&A

View full text Add to dashboard Cite

show abstract

“…Besides the wide spreading of SEPs, other interesting characteristics of this SEP event have been discussed, such as the significant depletion of SEPs associated with the interaction between the shock and a magnetic structure by Giacalone et al (2021), the similarity and differences of ion spectra at four spacecraft by Mason et al (2021), and the observation of inverted energy spectra due to the passage of previous CME (Lario et al 2021). More recently, the observation of this event near Mars as observed by Tianwen-1 has been reported by Fu et al (2022). Despite the fact that many observational studies have been devoted to this event, so far comprehensive modelling effort on this SEP event is still lacking.…”

Section: Introductionmentioning

confidence: 83%

Modelling the 2020 November 29 solar energetic particle event using the EUHFORIA and the iPATH model

Ding¹,

Wijsen²,

Li³

et al. 2022

Preprint

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Aims. We present the implementation of coupling the EUropean Heliospheric FORcasting Information Asset (EUHFORIA) and the improved Particle Acceleration and Transport in the Heliosphere (iPATH) model and simulate the widespread solar energetic particle (SEP) event of 2020 November 29. We compare the simulated time intensity profiles with measurements at Parker Solar Probe (PSP), the Solar Terrestrial Relations Observatory (STEREO)-A, SOlar and Heliospheric Observatory (SOHO) and Solar Orbiter (SolO). We focus on the influence of the history of shock acceleration on the varying SEP time intensity profiles and investigate the underlying causes in the origin of this widespread SEP event.Methods. We simulate a magnetized coronal mass ejection (CME) propagating in the data-driven solar wind with the EUHFORIA code. The CME is initiated by using the linear force-free spheromak module of EUHFORIA. Shock parameters and a 3D shell structure are computed from EUHFORIA as inputs for the iPATH model. Within the iPATH model, the steady-state solution of particle distribution assuming diffuse shock acceleration is obtained at the shock front. The subsequent SEP transport is described by the focused transport equation using the backward stochastic differential equation method with perpendicular diffusion included. Results. The temporal evolution of shock parameters and particle fluxes during this event are examined. We find that adopting a realistic solar wind background can significantly impact the expansion of the shock and consequently the shock parameters. Time intensity profiles with an energetic storm particle event at PSP are well reproduced from the simulation. In addition, the simulated and observed time intensity profiles of protons show a similar two-phase enhancement at STA. These results illustrate that modelling a shock using a realistic solar wind is crucial in determining the characteristics of SEP events. The decay phase of the modelled time intensity profiles at Earth agrees well with observations, indicating the importance of perpendicular diffusion in widespread SEP events. Taking into account the possible large curved magnetic field line connecting to SolO, the modelled time intensity profiles show good agreement with the observation. We suggest that the largely distorted magnetic field lines due to a stream interaction region may be a key factor in understanding the observed SEPs at SolO in this event.

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Particle radiation environment in the heliosphere: Status, limitations, and recommendations

Guo,

Wang,

Whitman

et al. 2024

Advances in Space Research

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First Report of a Solar Energetic Particle Event Observed by China’s Tianwen-1 Mission in Transit to Mars

Cited by 6 publications

References 56 publications

Modeling the 2020 November 29 solar energetic particle event using EUHFORIA and iPATH models

Modeling the 2020 November 29 solar energetic particle event using EUHFORIA and iPATH models

Modelling the 2020 November 29 solar energetic particle event using the EUHFORIA and the iPATH model

Particle radiation environment in the heliosphere: Status, limitations, and recommendations

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