The Quantitative Relation of the Time Profiles of Intensities in the Well-connected Solar Energetic Particle Events

Wang, Yang; Lyu, Dan; Wu, Xinghui; Qin, Gang

doi:10.3847/1538-4357/ac99da

Cited by 5 publications

(4 citation statements)

References 24 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…Therefore, we can define the spacecraft that observes the earliest peak time and the highest peak intensity as the highest peak intensity spacecraft in every energetic proton event, abbreviated as HPI spacecraft, which is the same for all energy channels. In a previous study (Wang et al 2022), we statistically studied the peak times of STEREO A, STEREO B, and SOHO spacecraft for 13-64 MeV energetic proton events from 2010-2014. In Figure 1, by the end of 2010, the longitudinal difference between STEREO A and STEREO B exceeded 130°.…”

Section: Energetic Proton Events Observed By Multiple Spacecraftmentioning

confidence: 99%

The Crucial Role of Perpendicular Diffusion in the Longitude Distribution of >10 MeV Solar Energetic Protons

Wang,

Qin

2023

ApJ

Self Cite

View full text Add to dashboard Cite

Gradual solar proton events are thought to consist of solar components originating near the Sun and interplanetary components associated with interplanetary shocks, and the role of interplanetary shocks is considered to be crucial in supplying particles to regions that are not magnetically connected to the solar source region. We calculate the ratios of the peak intensities for the four energy channels (13–16, 20–25, 32–40, and 40–64 MeV) and compare the ratios observed by multiple spacecraft at different locations. We often find that the ratio of peak intensities observed at different locations in the same event remains almost constant as the energy varies. In other words, the ratio of peak intensities from the different energy channels remains almost constant as the position of the spacecraft changes. The phenomenon implies that in many gradual events, energetic particles observed at different locations are mainly composed of solar components that undergo perpendicular diffusion in both the vicinity of the Sun and the interplanetary space, and that perpendicular diffusion is the main factor enabling energetic particles to be observed in regions without magnetic connection to the solar source region.

show abstract

Section: Energetic Proton Events Observed By Multiple Spacecraftmentioning

confidence: 99%

The Crucial Role of Perpendicular Diffusion in the Longitude Distribution of >10 MeV Solar Energetic Protons

Wang,

Qin

2023

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…There are more SEP events during solar maximum than during solar minimum. SEP events are commonly investigated through spacecraft observations (e.g., Tan et al 2009;McComas et al 2019;Thampi et al 2019;Wang et al 2021Wang et al , 2022 and numerical simulations with SEP transport and acceleration modeling (e.g., Ruffolo 1995;Dröge 2000;Qin et al 2006;Luhmann et al 2007;Zhang et al 2009;Dresing et al 2012;Wang et al 2012;Kozarev et al 2013;Hu et al 2018;Wijsen et al 2019aWijsen et al , 2019bWei et al 2019;Wu & Qin 2020;Wijsen et al 2021Wijsen et al , 2022. In order to study SEPs with transport modeling, one needs to have the solar wind velocity and solar wind background magnetic field.…”

Section: Introductionmentioning

confidence: 99%

Modeling the Transport of Solar Energetic Particles in a Corotating Interaction Region

Zhong,

Qin,

2024

ApJ

View full text Add to dashboard Cite

We present a new three-dimensional (3D) magnetohydrodynamic (MHD) model and a new 3D energetic particle transport (EPT) model. The 3D MHD model numerically solves the ideal MHD equations using the relaxing total variation diminishing scheme. In the 3D MHD simulations, we use simple boundary conditions with a high-speed flow, and we can clearly identify a corotating interaction region (CIR) with the characteristics of forward shock and reverse shock. The 3D EPT model solves the Fokker–Planck transport equation for the solar energetic particles (SEPs) using backward stochastic processes, with the magnetic field and solar wind velocity field from MHD results. For comparison, the 3D EPT model results with Parker fields are also obtained. We investigate the transport of SEPs with particle sources and observers in different positions in MHD fields with a CIR, and we compare the results with those in the Parker fields. Our simulation results show that the compression region with local enhancement of the magnetic field, i.e., CIR, can act as a barrier to scatter energetic particles back, and particles can struggle to diffuse through the strong magnetic field regions. Usually, a normal anisotropy profile is commonly present in SEP simulation results with Parker fields, and it is also typically present in that with MHD fields. However, because of the compression region of the magnetic field, energetic particles may exhibit anomalous anisotropy. This result may be used to replicate the spacecraft observation phenomena of the anomalous anisotropy.

show abstract

“…During the propagation of SEPs in interplanetary space, some researchers have used the focused transport equation, solving it directly or backward in time, based on the method of the stochastic differential equation. For example, Wang et al 2022a) used a SEP source with two free parameters and a diffusion model of the propagation of SEPs in interplanetary space (Krimigis 1965). They compared their calculation results with measurements in four energy channels in 59 events.…”

Section: Introductionmentioning

confidence: 99%

Formation of the Injection Function of Solar Energetic Particles in Gradual Events

Petukhov,

Petukhova,

Petukhov

2023

ApJ

View full text Add to dashboard Cite

We present a model for solar energetic particle injection into interplanetary space in gradual events, in which particle acceleration occurs in a limited region of the solar atmosphere. The distribution function of particles accelerated by the diffusion mechanism is calculated. The flux of injected solar energetic particles is determined as a function of time and energy. We provide an explanation of the characteristic properties of the injection function and their dependence on the particle energy. Comparing the calculation results with ground-based measurements in the 2001 April 15 event shows a rough agreement with the particle density as a function of time and good agreement with the spectrum of maximum intensity values.

show abstract

The Quantitative Relation of the Time Profiles of Intensities in the Well-connected Solar Energetic Particle Events

Cited by 5 publications

References 24 publications

The Crucial Role of Perpendicular Diffusion in the Longitude Distribution of >10 MeV Solar Energetic Protons

The Crucial Role of Perpendicular Diffusion in the Longitude Distribution of >10 MeV Solar Energetic Protons

Modeling the Transport of Solar Energetic Particles in a Corotating Interaction Region

Formation of the Injection Function of Solar Energetic Particles in Gradual Events

Contact Info

Product

Resources

About