On the Seed Population of Solar Energetic Particles in the Inner Heliosphere

Wijsen, Nicolas; Li, Gang; Ding, Zheyi; Lario, D.; Poedts, Stefaan; Filwett, Rachael; Allen, R. C.; Dayeh, M. A.

doi:10.1029/2022ja031203

Cited by 13 publications

(18 citation statements)

References 74 publications

(114 reference statements)

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“…We then describe how the particle acceleration and transport is followed from the vicinity of the CIR reverse shock to an observer. This follows closely to recent works by Wijsen et al (2021Wijsen et al ( , 2023. In Section 3, we present a comparative analysis for cases with and without perpendicular diffusion.…”

Section: Introductionmentioning

confidence: 60%

“…All analyses are done in the equatorial plane, as in the recent work by Wijsen et al (2023). Figure 1(a) displays the radial velocity of the solar wind, V r .…”

Section: Resultsmentioning

confidence: 99%

“…Figure 1(c) shows the parallel mean free path λ ∥ for 50 keV protons. Away from the reverse shock, λ ∥ increases with the heliocentric distance, reflecting the gyrofrequency of particles and their wave-particle resonance conditions with the background magnetic field (Wijsen et al 2023). Note that in the rarefaction region particles exhibit a larger parallel mean free path.…”

Section: Resultsmentioning

confidence: 99%

“…These terms collectively model the influence of a fluctuating magnetic field, δB, on particle transport. Additionally, we adopt the assumption by Wijsen et al (2023) for the radial dependence of δB 2 /B 2 . Following in describing D μμ using the the quasi-linear theory (QLT; Jokipii 1966) and κ ⊥ from κ ∥ using the NLGC theory (Shalchi et al 2010), we can obtain the…”

Section: Modelmentioning

confidence: 99%

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Modeling Ion Acceleration and Transport in Corotating Interaction Regions: The Mass-to-charge Ratio Dependence of the Particle Spectrum

Ding,

Li,

Wijsen

et al. 2024

ApJL

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We investigate the role of perpendicular diffusion in shaping the energetic ion spectrum in corotating interaction regions (CIRs), focusing on its mass-to-charge (A/Q) ratio dependence. We simulate a synthetic CIR using the EUropean Heliospheric FORecasting Information Asset and model the subsequent ion acceleration and transport by solving the focused transport equation incorporating both parallel and perpendicular diffusion. Our results reveal distinct differences in ion spectra between scenarios with and without perpendicular diffusion. In the absence of perpendicular diffusion, ion spectra near CIRs show a strong (A/Q) ϵ dependence with ϵ depending on the turbulence spectral index, agreeing with theoretical predictions. In contrast, the incorporation of perpendicular diffusion, characterized by a weak A/Q dependence, leads to similar spectra for different ion species. This qualitatively agrees with observations of energetic particles in CIRs.

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Section: Introductionmentioning

confidence: 60%

“…All analyses are done in the equatorial plane, as in the recent work by Wijsen et al (2023). Figure 1(a) displays the radial velocity of the solar wind, V r .…”

Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Section: Modelmentioning

confidence: 99%

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Modeling Ion Acceleration and Transport in Corotating Interaction Regions: The Mass-to-charge Ratio Dependence of the Particle Spectrum

Ding,

Li,

Wijsen

et al. 2024

ApJL

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“…First, the spectral indices of the seed population may differ between events and even differ during an individual event. A recent study by Wijsen et al (2023) suggests that the spectral indices of the seed population can be strongly altered by velocity shears in the solar wind (e.g., corotating interaction regions). As discussed in Appendix A, the injection efficiency sensitively depends on the spectral indices of the seed population.…”

Section: Resultsmentioning

confidence: 99%

The East‐West Asymmetry of Particle Intensity in Energetic Storm Particle Events

Ding

Dueñas

et al. 2023

JGR Space Physics

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Solar energetic particles (SEP) accelerated by the coronal mass ejection (CME) shocks are known as gradual SEP events. During gradual events, the enhancements of particle intensity associated with the passage of the interplanetary shock near spacecraft are referred to as energetic storm particle (ESP) events (Bryant et al., 1962). The properties of ESP events observed at 1 au, and their correlations with shock properties and upstream conditions have been widely studied. For instance, M. I. Desai et al. (2003) found significant correlations between the interplanetary shock abundances and the ambient superthermal ions. Reames (2012) suggested that the shock speed correlates best with the particle intensities in ESP events. Additionally, Ebert et al. ( 2016) examined seven multiple-spacecraft ESP events and found that the peak intensities near the shock nose are larger than at the flank of the shock. More recently, Santa Fe Dueñas et al. (2022) showed that heavy ion peak intensities and spectra at 1 au are organized by longitude relative to their source flare location, which appeared to have an East-West asymmetric distribution of the peak intensity. This asymmetry refers to the difference of particle intensities between the eastern and the western shock flank. Unlike the East-West asymmetry of particle intensity in large SEP events, which is affected by the extended shock acceleration and the transport effects (e.g., Lario et al., 2006;Strauss et al., 2017;Xie et al., 2019), ESP events are typically interpreted as a direct consequence of a local shock acceleration process. Thus, the East-West asymmetry of the particle intensity in ESP events may provide important insights into the underlying acceleration mechanism.

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Solar Wind With Field Lines and Energetic Particles (SOFIE) Model: Application to Historical Solar Energetic Particle Events

Zhao,

Sokolov,

Gombosi

et al. 2024

Space Weather

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In this paper, we demonstrate the applicability of the data‐driven solar energetic particle (SEP) model, SOlar‐wind with FIeld‐lines and Energetic‐particles (SOFIE), to simulate the acceleration and transport processes of SEPs and make forecast of the energetic proton flux at energies ≥10 MeV that will be observed near 1 AU. The SOFIE model is built upon the Space Weather Modeling Framework developed at the University of Michigan. In SOFIE, the background solar wind plasma in the solar corona and interplanetary space is calculated by the Stream‐Aligned Aflvén Wave Solar‐atmosphere Model(‐Realtime) driven by the near‐real‐time hourly updated Global Oscillation Network Group solar magnetograms. In the background solar wind, coronal mass ejections (CMEs) are launched by placing an force‐imbalanced magnetic flux rope on top of the parent active region, using the Eruptive Event Generator using Gibson‐Low model. The acceleration and transport processes are modeled by the Multiple‐Field‐Line Advection Model for Particle Acceleration. In this work, nine SEP events (Solar Heliospheric and INterplanetary Environment challenge/campaign events) are modeled. The three modules in SOFIE are validated and evaluated by comparing with observations, including the steady‐state background solar wind properties, the white‐light image of the CMEs, and the flux of solar energetic protons, at energies of ≥10 MeV.

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On the Seed Population of Solar Energetic Particles in the Inner Heliosphere

Cited by 13 publications

References 74 publications

Modeling Ion Acceleration and Transport in Corotating Interaction Regions: The Mass-to-charge Ratio Dependence of the Particle Spectrum

Modeling Ion Acceleration and Transport in Corotating Interaction Regions: The Mass-to-charge Ratio Dependence of the Particle Spectrum

The East‐West Asymmetry of Particle Intensity in Energetic Storm Particle Events

Solar Wind With Field Lines and Energetic Particles (SOFIE) Model: Application to Historical Solar Energetic Particle Events

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