2001
DOI: 10.1046/j.1365-8711.2001.04851.x
|View full text |Cite
|
Sign up to set email alerts
|

Particle acceleration by ultrarelativistic shocks: theory and simulations

Abstract: We consider the acceleration of charged particles near ultrarelativistic shocks, with Lorentz factor . We present simulations of the acceleration process and compare these with results from semi‐analytical calculations. We show that the spectrum that results from acceleration near ultrarelativistic shocks is a power law, , with a nearly universal value for the slope of this power law. We confirm that the ultrarelativistic equivalent of the Fermi acceleration at a shock differs from its non‐relativistic cou… Show more

Help me understand this report
View preprint versions

Search citation statements

Order By: Relevance

Paper Sections

Select...
2
1
1
1

Citation Types

103
563
5

Year Published

2003
2003
2016
2016

Publication Types

Select...
4
2
2

Relationship

0
8

Authors

Journals

citations
Cited by 579 publications
(671 citation statements)
references
References 65 publications
(86 reference statements)
103
563
5
Order By: Relevance
“…This is in agreement with numerical simulations of relativistic shocks, which have demonstrated that diffusive shock acceleration forms such power-law spectra (Achterberg et al 2001;Spitkovsky 2008;Summerlin & Baring 2012). Therefore, shocks are frequently used to explain blazar flaring activities.…”
Section: Introductionsupporting
confidence: 89%
See 1 more Smart Citation
“…This is in agreement with numerical simulations of relativistic shocks, which have demonstrated that diffusive shock acceleration forms such power-law spectra (Achterberg et al 2001;Spitkovsky 2008;Summerlin & Baring 2012). Therefore, shocks are frequently used to explain blazar flaring activities.…”
Section: Introductionsupporting
confidence: 89%
“…Such polarization variations with no obvious flares are consistent with some observations (e.g., Itoh et al 2013;Jorstad et al 2013). However, Kirk et al (2000) and Achterberg et al (2001) have shown that for relativistic shocks, the hardest obtainable particle power-law index is approximately…”
Section: Discussion and Summarymentioning
confidence: 99%
“…2, and show that in this application one requiresθ < 0.1/γ shock . Our results are quite consistent with those of Achterberg et al (2001), who used a diffusive angular step ∆θ st ≤ 0.1/γ shock . Figure 2.…”
Section: Application To Relativistic Shock Accelerationsupporting
confidence: 91%
“…Clearly, Monte Carlo simulation by a random walk with mean free path λ and large-angle scattering is inappropriate here, and in Monte Carlo simulations of relativistic shock acceleration at parallel shocks Achterberg et al (2001) consider instead the diffusion of a particle's direction for a given angular diffusion coefficient D θ (rad 2 s −1 ). Similarly, for a given spatial diffusion coefficient D, Protheroe (2001) and Meli & Quenby (2001) adopt a random walk with a smaller mean free path,l ≪ λ, followed by scattering at each step by a small angle with mean deflection ,θ < 1/γ shock .…”
Section: Introductionmentioning
confidence: 99%
“…In a finite shock, high-energy particles far upstream from the subshock have a high probability of escaping since the level of self-generated turbulence must decrease with upstream distance from the subshock. Particle escape could as well occur downstream from the subshock, as assumed in relativistic shock calculations by Achterberg et al (2001) and Warren et al (2015), or from the sides, as might be important in jets. How escape occurs will depend on the detailed geometry of the shock but all these scenarios produce a corresponding p max with no important differences from what we describe here.…”
Section: Details Of Modelmentioning
confidence: 97%