Combining MHD and kinetic modelling of solar flares

Gordovskyy, Mykola; Browning, Philippa; Pinto, Rui

doi:10.1016/j.asr.2018.09.024

Cited by 13 publications

(5 citation statements)

References 133 publications

(144 reference statements)

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“…However, kinetic approaches, which can consistently account for nonthermal particles, cannot be realistically used at large scales. Hence, an approach combining MHD and kinetic simulations is often used (see, e.g., Gordovskyy et al 2019, for review and references). Hybrid fluid-kinetic methods can provide more rigorous and self-consistent description of energetic particles at large scales.…”

Section: Introductionmentioning

confidence: 99%

Forward Modeling of Particle Acceleration and Transport in an Individual Solar Flare

Gordovskyy¹,

Browning²,

Inoue

et al. 2020

ApJ

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The aim of this study is to generate maps of the hard X-ray emission produced by energetic electrons in a solar flare and compare them with observations. The ultimate goal is to test the viability of the combined MHD/test-particle approach for data-driven modeling of active events in the solar corona and their impact on the heliosphere. Based on an MHD model of X-class solar flare observed on 2017 September 8, we calculate trajectories of a large number of electrons and protons using the relativistic guiding-center approach. Using the obtained particle trajectories, we deduce the spatial and energy distributions of energetic electrons and protons, and calculate bremsstrahlung hard X-ray emission using the "thin-target" approximation. Our approach predicts some key characteristics of energetic particles in the considered flare, including the size and location of the acceleration region, energetic particle trajectories and energy spectra. Most importantly, the hard X-ray bremsstrahlung intensity maps predicted by the model are in good agreement with those observed by RHESSI. Furthermore, the locations of proton and electron precipitation appear to be close to the sources of helioseismic response detected in this flare. Therefore, the adopted approach can be used for observationally driven modeling of individual solar flares, including manifestations of energetic particles in the corona, as well as the inner heliosphere.

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Section: Introductionmentioning

confidence: 99%

Forward Modeling of Particle Acceleration and Transport in an Individual Solar Flare

Gordovskyy¹,

Browning²,

Inoue

et al. 2020

ApJ

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“…The MHD models are then used to trace trajectories of large numbers (∼10 6 ) of test electrons and protons using relativistic guiding-center motion equations with the field values calculated for each particle position at each time step using fourlinear interpolation (in the [X, Y, Z, t] space). These calculations are performed using the 3D GCA code (Gordovskyy & Browning 2011;Gordovskyy et al 2014Gordovskyy et al , 2019.…”

Section: Main Equations and Numerical Setupmentioning

confidence: 99%

Particle Acceleration and Their Escape into the Heliosphere in Solar Flares with Open Magnetic Field

Gordovskyy

Browning

Kusano

et al. 2023

ApJ

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Energetic particle populations in the solar corona and in the heliosphere appear to have different characteristics even when produced in the same solar flare. It is not clear what causes this difference: properties of the acceleration region, the large-scale magnetic field configuration in the flare, or particle transport effects, such as scattering. In this study, we use a combination of magnetohydrodynamic and test-particle approaches to investigate magnetic reconnection, particle acceleration, and transport in two solar flares: an M-class flare on 2013 June 19, and an X-class flare on 2011 September 6. We show that in both events, the same regions are responsible for the acceleration of particles remaining in the coronal and being ejected toward the heliosphere. However, the magnetic field structure around the acceleration region acts as a filter, resulting in different characteristics (such as energy spectra) acquired by these two populations. We argue that this effect is an intrinsic property of particle acceleration in the current layers created by the interchange reconnection, and therefore, may be ubiquitous, particularly, in noneruptive solar flares with substantial particle emission into the heliosphere.

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“…Magnetic reconnection (MR) is a fundamental process that converts magnetic energy into plasma thermal energy and kinetic energy [1]. It plays a crucial role in explaining high-energy phenomena in astrophysical environments [2,3], such as the interaction between the solar wind and the magnetosphere [4,5], solar flares [6], gamma-ray bursts [7][8][9], and pulsar wind nebulae [10][11][12]. In laboratory experiments [13][14][15][16] and Particle-In-Cell (PIC) simulations [17][18][19], MR driven by intense lasers has been extensively studied.…”

Section: Introductionmentioning

confidence: 99%

Electron acceleration in the electron dissipation region of asymmetrical magnetic reconnection driven by ultra-intensity lasers

Zhang,

Ping,

et al. 2024

Plasma Phys. Control. Fusion

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We performed 3D Particle-In-Cell simulations to study electron acceleration in the electron dissipation region of asymmetrical electron magnetic reconnection driven by ultra-intensity lasers, which is similar to the Earth's magnetosphere reconnection process. Within the electron dissipation region, electrons exhibit a nonthermal distribution, and as the asymmetry increases, the power-law spectrum becomes steeper. Remarkably, the electron spectrum closely resembles a delta distribution, arising from the intense acceleration imparted by the reconnection electric field near the X-line. Both parallel electric field acceleration and the Betatron acceleration mechanism play pivotal roles in this reconnection process. Furthermore, as the magnetic reconnection asymmetry intensifies, the parallel electric acceleration mechanism becomes stronger near the X-point region, whereas the Betatron acceleration mechanism wanes, primarily concentrated in the outflow region.

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Combining MHD and kinetic modelling of solar flares

Cited by 13 publications

References 133 publications

Forward Modeling of Particle Acceleration and Transport in an Individual Solar Flare

Forward Modeling of Particle Acceleration and Transport in an Individual Solar Flare

Particle Acceleration and Their Escape into the Heliosphere in Solar Flares with Open Magnetic Field

Electron acceleration in the electron dissipation region of asymmetrical magnetic reconnection driven by ultra-intensity lasers

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