PIC simulation methods for cosmic radiation and plasma instabilities

Pohl, Martin; Hoshino, Masahiro; Niemiec, J.

doi:10.1016/j.ppnp.2019.103751

Cited by 38 publications

(21 citation statements)

References 335 publications

(412 reference statements)

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“…The simulations were carried out using a parallelized EM PIC code, TRISTAN-MP (Buneman 1993;Spitkovsky 2005) . Interpreting the results of our PIC simulations could be limited by numerical noises and aliases due to a finite number of macroparticles on discretized grids (e.g., Pohl et al 2020). However, we expect that the overall results of the PIC simulations are reasonably converged, judging from the previous studies (Guo et al 2014b;Kang et al 2019;Kim et al 2020).…”

Section: Numerical Setupmentioning

confidence: 99%

“…Hence, this kind of analysis on kinetic scales can provide crucial insights for theoretical modelings and/or larger-scale simulations of particle acceleration at weak high-β shocks. However, one of the limitations of PIC simulations is that they can follow kinetic plasma processes mainly at the low end of temporal and spatial scales owing to severe requirements of computational resources (e.g., Pohl et al 2020).…”

Section: Introductionmentioning

confidence: 99%

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Microinstabilities in the Transition Region of Weak Quasi-perpendicular Intracluster Shocks

Kim

Ryu

et al. 2021

ApJ

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Microinstabilities play important roles in both entropy generation and particle acceleration in collisionless shocks. Recent studies have suggested that in the transition region of quasi-perpendicular (Q ⊥ ) shocks in the high-beta (β = P gas /P B ) intracluster medium (ICM), the ion temperature anisotropy due to the reflected-gyrating ions could trigger the Alfvén ion cyclotron (AIC) instability and the ion-mirror instability, while the electron temperature anisotropy induced by magnetic field compression could excite the whistler instability and the electron-mirror instability. Adopting the numerical estimates for ion and electron temperature anisotropies found in the particle-incell (PIC) simulations of Q ⊥ shocks with sonic Mach numbers, M s = 2-3, we carry out a linear stability analysis for these microinstabilities. The kinetic properties of the microinstabilities and the ensuing plasma waves on both ion and electron scales are described for wide ranges of parameters, including β and the ion-to-electron mass ratio. In addition, the nonlinear evolution of the induced plasma waves are examined by performing 2D PIC simulations with periodic boundary conditions. We find that for β ≈ 20-100, the AIC instability could induce ion-scale waves and generate shock surface ripples in supercritical shocks above the AIC critical Mach number,. Also, electron-scale waves are generated primarily by the whistler instability in these high-β shocks. The resulting multiscale waves from electron to ion scales are thought to be essential in the electron injection to diffusive shock acceleration in Q ⊥ shocks in the ICM.

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Section: Numerical Setupmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Microinstabilities in the Transition Region of Weak Quasi-perpendicular Intracluster Shocks

Kim

Ryu

et al. 2021

ApJ

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“…A part of cascade energy can be lost due to plasma beam instabilities [60]. There have been many works modeling these collective plasma losses using Particle-In-Cell simulation methods (they are listed and reviewed in relation to cascade pair beams in Section 4.3 of [61]). However, as of yet there is no clear consensus on the extent of these losses in the context of extragalactic gamma-ray propagation from distant blazars.…”

Section: Discussionmentioning

confidence: 99%

Modeling Gamma-Ray SEDs and Angular Extensions of Extreme TeV Blazars from Intergalactic Proton-Initiated Cascades in Contemporary Astrophysical EGMF Models

Khalikov

2021

Universe

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The intrinsic spectra of some distant blazars known as “extreme TeV blazars” have shown a hint at an anomalous hardening in the TeV energy region. Several extragalactic propagation models have been proposed to explain this possible excess transparency of the Universe to gamma-rays starting from a model which assumes the existence of so-called axion-like particles (ALPs) and the new process of gamma-ALP oscillations. Alternative models suppose that some of the observable gamma-rays are produced in the intergalactic cascades. This work focuses on investigating the spectral and angular features of one of the cascade models, the Intergalactic Hadronic Cascade Model (IHCM) in the contemporary astrophysical models of Extragalactic Magnetic Field (EGMF). For IHCM, EGMF largely determines the deflection of primary cosmic rays and electrons of intergalactic cascades and, thus, is of vital importance. Contemporary Hackstein models are considered in this paper and compared to the model of Dolag. The models assumed are based on simulations of the local part of large-scale structure of the Universe and differ in the assumptions for the seed field. This work provides spectral energy distributions (SEDs) and angular extensions of two extreme TeV blazars, 1ES 0229+200 and 1ES 0414+009. It is demonstrated that observable SEDs inside a typical point spread function of imaging atmospheric Cherenkov telescopes (IACTs) for IHCM would exhibit a characteristic high-energy attenuation compared to the ones obtained in hadronic models that do not consider EGMF, which makes it possible to distinguish among these models. At the same time, the spectra for IHCM models would have longer high energy tails than some available spectra for the ALP models and the universal spectra for the Electromagnetic Cascade Model (ECM). The analysis of the IHCM observable angular extensions shows that the sources would likely be identified by most IACTs not as point sources but rather as extended ones. These spectra could later be compared with future observation data of such instruments as Cherenkov Telescope Array (CTA) and LHAASO.

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“…Here the color scale designates the fast magnetosonic Mach number. magnetosonic Mach number and , in stark contrast with some recent hybrid simulations (kinetic ions and fluid electrons), as summarized in the review [8].…”

Section: Pos(icrc2021)1311mentioning

confidence: 99%

Energy Balance at Interplanetary Shocks: In-situ Measurement of the Fraction in Supra-thermal and Energetic Ions with ACE and Wind

David¹,

Fraschetti²,

Giacalone³

et al. 2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

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The acceleration of charged particles by interplanetary shocks can drain a non-negligible fraction of the upstream ram pressure. For a sample of shocks observed in-situ at 1 AU by the ACE and Wind spacecraft, time-series of the non-Maxwellian components (supra-thermal and higher-energy) of the ion and electron energy spectra were acquired for each event. These were averaged for one hour before and after the time of the shock passage to determine their partial pressure. Using the MHD Rankine-Hugoniot jump conditions, we find that the fraction of the total upstream energy flux transferred to non-Maxwellian downstream particles is typically about 2-16%. Notably, our sample shows that neither the fast magnetosonic Mach number nor the angle between the shock normal and average upstream magnetic field are correlated with non-Maxwellian particle pressure.

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PIC simulation methods for cosmic radiation and plasma instabilities

Cited by 38 publications

References 335 publications

Microinstabilities in the Transition Region of Weak Quasi-perpendicular Intracluster Shocks

Microinstabilities in the Transition Region of Weak Quasi-perpendicular Intracluster Shocks

Modeling Gamma-Ray SEDs and Angular Extensions of Extreme TeV Blazars from Intergalactic Proton-Initiated Cascades in Contemporary Astrophysical EGMF Models

Energy Balance at Interplanetary Shocks: In-situ Measurement of the Fraction in Supra-thermal and Energetic Ions with ACE and Wind

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