Generation of Magnetic Fields in the Relativistic Shock of Gamma‐Ray Burst Sources

Medvedev, Mikhail V.; Loeb, Abraham

doi:10.1086/308038

Cited by 858 publications

(967 citation statements)

References 45 publications

Supporting

Mentioning

931

Contrasting

Order By: Relevance

“…Jitter radiation, which is the emission of relativistic electrons in a random and small-scale magnetic field, has been applied to GRB research (Medvedev 2000(Medvedev , 2006. The random and small-scale magnetic field can be generated by Weibel instability (Medvedev & Loeb 1999). Alternatively, we propose that the turbulent cascade process can also produce the random and small-scale magnetic field (Mao & Wang 2007.…”

Section: Introductionmentioning

confidence: 99%

JITTER SELF-COMPTON PROCESS: GeV EMISSION OF GRB 100728A

Mao

Wang

2012

ApJ

View full text Add to dashboard Cite

Jitter radiation, the emission of relativistic electrons in a random and small-scale magnetic field, has been applied to explain the gamma-ray burst (GRB) prompt emission. The seed photons produced from jitter radiation can be scattered by thermal/nonthermal electrons to the high-energy bands. This mechanism is called jitter self-Compton (JSC) radiation. GRB 100728A, which was simultaneously observed by Swift and Fermi, is a great example to constrain the physical processes of jitter and JSC. In our work, we utilize jitter/JSC radiation to reproduce the multiwavelength spectrum of GRB 100728A. In particular, due to JSC radiation, the powerful emission above the GeV band is the result of those jitter photons in the X-ray band scattered by the relativistic electrons with a mixed thermal-nonthermal energy distribution. We also combine the geometric effect of microemitters to the radiation mechanism, such that the "jet-in-jet" scenario is considered. The observed GRB duration is the result of summing up all of the contributions from those microemitters in the bulk jet.

show abstract

Section: Introductionmentioning

confidence: 99%

JITTER SELF-COMPTON PROCESS: GeV EMISSION OF GRB 100728A

Mao

Wang

2012

ApJ

View full text Add to dashboard Cite

show abstract

“…Here we show that such seed fields can originate from the Weibel instabilities (Weibel 1959). These instabilities are driven by various kinetic anisotropies, e.g., heating flows, shocks and interpenetrating plasma shells, and generate long-lived quasistatic magnetic fields providing plausible explanations for the origin of cosmological magnetic field (Schlickeiser & Shukla 2003) or the magnetic boosts in astrophysical sources (GRBs, SNRs) of nonthermal radiation (Medvedev & Loeb 1999).…”

Section: Introductionmentioning

confidence: 77%

“…The mode with the largest growth rate, Γ m ax (k m ax ), dominates and sets the characteristic length scale of the magnetic field fluctuations, λ ∼ k −1 m ax at the saturation. Particles free streaming across the excited magnetic field lines is suppressed once the particle's gyroradius ρ = v/Ω m ax = eB m ax /(mc) becomes comparable to the length scale of the magnetic field fluctuations, k −1 m ax , yielding (Medvedev & Loeb 1999) Schlickeiser & Shukla 2003, Lazar et al 2009.…”

Section: Weibel Instabilitiesmentioning

confidence: 99%

Cosmological magnetic field seeds produced by the Weibel instabilities

2010

View full text Add to dashboard Cite

Abstract. The source of the cosmological magnetic field is still unknown because the widely invoked dynamo processes are only able to regenerate and amplify some initial magnetic field seeds. In the hot and highly ionized intergalactic matter such magnetic field seeds can easily be produced by the (electro-)magnetic instabilities of Weibel type. Here we discuss suplementary mechanisms that can make these Weibel created fields to evolve at large scales presently observed in galaxies and clusters and can also enhance these magnetic field seeds after the dissipation.

show abstract

“…Accordingly, such aperiodic growing fluctuations surely play an important role in GRBs that are already magnetized due to internal shocks, as predicted by Medvedev & Loeb (1999).…”

Section: Introductionmentioning

confidence: 81%

Plasma Instabilities in Gamma‐Ray Bursts: Neutral Points and the Effect of Mode Coupling

Tautz

Lerche

2006

ApJ

View full text Add to dashboard Cite

The method of determining neutral points, corresponding to vanishing frequency in wavenumber space, is applied to the case of gamma-ray bursts (GRBs) to determine low-frequency instabilities. If a particular particle distribution function permits the existence of neutral points, instability is guaranteed on one side or the other of the neutral point. By using the rest frame of the GRB jets, only perpendicular particle motion has to be taken into account. The discussion is limited to the cases of a monoenergetic electron-proton plasma with stationary protons and also to a symmetric electronpositron plasma. In the limiting case of wave propagation perpendicular to a homogeneous background magnetic field, taken to be parallel to the streaming direction of the jet, it is shown that to lowest order in the wave frequency, unstable aperiodic fluctuations occur that grow very rapidly on timescales comparable to or smaller than the characteristic times of the GRB, leading to the conclusion that the jets most likely consist mainly of electron-proton plasmas for the cases investigated. Furthermore, high electron Lorentz factors, as well as the coupling effect between longitudinal and transverse modes, are shown to stabilize the system.

show abstract

Generation of Magnetic Fields in the Relativistic Shock of Gamma‐Ray Burst Sources

Cited by 858 publications

References 45 publications

JITTER SELF-COMPTON PROCESS: GeV EMISSION OF GRB 100728A

JITTER SELF-COMPTON PROCESS: GeV EMISSION OF GRB 100728A

Cosmological magnetic field seeds produced by the Weibel instabilities

Plasma Instabilities in Gamma‐Ray Bursts: Neutral Points and the Effect of Mode Coupling

Contact Info

Product

Resources

About