Electron plasma wake field acceleration in solar coronal and chromospheric plasmas

Tsiklauri, David

doi:10.1063/1.4990560

Cited by 8 publications

(6 citation statements)

References 31 publications

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“…Here we argue that in some laboratory, see e.g. Figure 1 from Corde et al [16], and probably most astrophysical situations such as jets in the vicinity of black holes [11,12] and flares in solar atmosphere [13], plasma wakefield acceleration of electrons is one dimensional. Namely, variation transverse to the beam's motion can be ignored.…”

Section: Discussionmentioning

confidence: 70%

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Differences in 1D electron plasma wake field acceleration in MeV versus GeV and linear versus blowout regimes

Tsiklauri

2018

Physics of Plasmas

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In some laboratory and most astrophysical situations plasma wake-field acceleration of electrons is one dimensional, i.e. variation transverse to the beam's motion can be ignored. Thus, one dimensional (1D), particle-in-cell (PIC), fully electromagnetic simulations of electron plasma wake field acceleration are conducted in order to study the differences in electron plasma wake field acceleration in MeV versus GeV and linear versus blowout regimes. First, we show that caution needs to be taken when using fluid simulations, as PIC simulations prove that an approximation for an electron bunch not to evolve in time for few hundred plasma periods only applies when it is sufficiently relativistic. This conclusion is true irrespective of the plasma temperature. We find that in the linear regime and GeV energies, the accelerating electric field generated by the plasma wake is similar to the linear and MeV regime. However, because GeV energy driving bunch stays intact for much longer time, the final acceleration energies are much larger in the GeV energies case. In the GeV energy range and blowout regime the wake's accelerating electric field is much larger in amplitude compared to the linear case and also plasma wake geometrical size is much larger. Thus, the correct positioning of the trailing bunch is needed to achieve the efficient acceleration. For the considered case, optimally there should be approximately (90 − 100)c/ωpe distance between trailing and driving electron bunches in the GeV blowout regime.

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Section: Discussionmentioning

confidence: 70%

“…Good progress has been made in applying PWFA concepts to astrophysical plasmas. Including supermassive black hole [11,12], and solar atmosphere [13] contexts.…”

Section: Introductionmentioning

confidence: 99%

Differences in 1D electron plasma wake field acceleration in MeV versus GeV and linear versus blowout regimes

Tsiklauri

2018

Physics of Plasmas

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“…larger relative beam densities, the "wave+wave, beam+wave" energy transfer processes are more important (E. Kontar 2022, private communication), which can be understood as the result of more ion-acoustic turbulence present to enhance wave+wave processes. At very large beam density, fluid and PIC simulations (Bera et al 2015(Bera et al , 2020 of ultrarelativistic, monoenergetic beams instigate additional acceleration through the plasma wakefield effects that have only recently been considered in the context of solar/stellar flares (Tsiklauri 2017).…”

Section: Discussionmentioning

confidence: 99%

Bridging High-density Electron Beam Coronal Transport and Deep Chromospheric Heating in Stellar Flares

Kowalski

2023

ApJL

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The optical and near-ultraviolet (NUV) continuum radiation in M-dwarf flares is thought to be the impulsive response of the lower stellar atmosphere to magnetic energy release and electron acceleration at coronal altitudes. This radiation is sometimes interpreted as evidence of a thermal photospheric spectrum with T ≈ 104 K. However, calculations show that standard solar flare coronal electron beams lose their energy in a thick target of gas in the upper and middle chromosphere (log10 column mass/[g cm−2] ≲ −3). At larger beam injection fluxes, electric fields and instabilities are expected to further inhibit propagation to low altitudes. We show that recent numerical solutions of the time-dependent equations governing the power-law electrons and background coronal plasma (Langmuir and ion-acoustic) waves from Kontar et al. produce order-of-magnitude larger heating rates than those that occur in the deep chromosphere through standard solar flare electron beam power-law distributions. We demonstrate that the redistribution of beam energy above E ≳ 100 keV in this theory results in a local heating maximum that is similar to a radiative-hydrodynamic model with a large, low-energy cutoff and a hard power-law index. We use this semiempirical forward-modeling approach to produce opaque NUV and optical continua at gas temperatures T ≳ 12,000 K over the deep chromosphere with log10 column mass/[g cm−2] of −1.2 to −2.3. These models explain the color temperatures and Balmer jump strengths in high-cadence M-dwarf flare observations, and they clarify the relation among atmospheric, radiation, and optical color temperatures in stellar flares.

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“…In terms of theoretical work, till date, both linear and nonlinear theory in 1-D has been well established to examine PWFA scheme for several driver configurations over a wide range of beam parameters [16][17][18][19]. Numerical simulations using both fluid [19] and Particle-In-Cell (PIC) [24] technique for 1-D case have also been carried out. In 2-D, the theoretical studies for the excitation of wakefield have been done only in the linear regime and for specific set of beam configurations [20,21].…”

Section: Introductionmentioning

confidence: 99%

“…OSIRIS, EPOCH, QUICK-PIC etc.) [23][24][25]. These PIC simulations compute the trajectories of billions of particles for hundreds of plasma periods.…”

Section: Introductionmentioning

confidence: 99%

Fluid simulation of relativistic electron beam driven wakefield in a cold plasma

2015

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Fluid simulations, which are considerably simpler and faster, have been employed to study the behavior of the wake field driven by a relativistic rigid beam in a 2-D cold plasma. When the transverse dimensions of the beam is chosen to be much larger than its longitudinal extent, a good agreement with our previous 1-D results [Physics of Plasmas 22, 073109 (2015)] are observed for both under-dense and over-dense beams. When the beam is overdense and its transverse extent is smaller or close to the longitudinal extension, the 2-D blow-out structure, observed in PIC simulations and analytically modeled by Lu et al. [Phys. Rev. Lett., 96, 165002 (2006)] are recovered. For quantitative assessment of particle acceleration in such a wake potential structure test electrons are employed. It is shown that the maximum energy gained by the test electrons placed at the back of the driver beam of energy ∼ 28.5 GeV, reaches up to 2.6 GeV in a 10 cm long plasma. These observations are consistent with the experimental results presented in ref. [Phys. Rev. Lett. 95, 054802 (2005)]. It is also demonstrated that the energy gained by the test electrons get doubled (∼ 5.2 GeV) when the test particles are placed near the axis at the end of the first blowout structure.

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Electron plasma wake field acceleration in solar coronal and chromospheric plasmas

Cited by 8 publications

References 31 publications

Differences in 1D electron plasma wake field acceleration in MeV versus GeV and linear versus blowout regimes

Differences in 1D electron plasma wake field acceleration in MeV versus GeV and linear versus blowout regimes

Bridging High-density Electron Beam Coronal Transport and Deep Chromospheric Heating in Stellar Flares

Fluid simulation of relativistic electron beam driven wakefield in a cold plasma

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