Turbulent amplification of magnetic field and diffusive shock acceleration of cosmic rays

By A. Bell. 2004

966 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/0fa82c36f3d9ef0e39f1af5a1ee1bfbb99fe0116

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Citations in the corpus

WEIBEL, TWO-STREAM, FILAMENTATION, OBLIQUE, BELL, BUNEMAN...WHICH ONE GROWS FASTER? (2009, methodology): “These modes are the present configuration analogs to the ones explained by Bell (2004, 2005).”
Cosmic-ray energy spectrum and composition up to the ankle - the case for a second Galactic component (2016, background): “Such strong fields may lead to proton acceleration up to energies close to the cut-o↵ energy obtain in our study (Bell 2004).”
FERMI-LAT DISCOVERY OF GeV GAMMA-RAY EMISSION FROM THE YOUNG SUPERNOVA REMNANT CASSIOPEIA A (2010, background): “Recent theoretical work indicates that the magnetic field can be largely amplified by streaming of CRs themselves, as an integral part of efficient CR acceleration at collisionless shocks (Bell & Lucek 2001; Bell 2004).”
Magnetic Fields in the Large-Scale Structure of the Universe (2011, background): “During the process of acceleration, it was shown that the upstream magnetic field can be amplified 15 nonlinearly by non-resonant growing modes (Bell 2004).”
PARTICLE ACCELERATION IN RELATIVISTIC MAGNETIZED COLLISIONLESS ELECTRON–ION SHOCKS (2010, background): “In this case, the electric current of “returning” ions can trig- 20 ger the so-called Bell’s instability (Bell 2004), which generates powerful circularly-polarized Alfvénic-type waves in the upstream.”
SPECTRUM OF GALACTIC COSMIC RAYS ACCELERATED IN SUPERNOVA REMNANTS (2010, background): “The work of Bell (2004) demonstrated that a very large ran- dom magnetic field δB ≫ Bism (where Bism≈5µG is the average interstellar field upstream of the shock) can be generated by a cosmic-ray streaming instability in the precursor of strong shocks.”
THE FIRST FERMI LAT SUPERNOVA REMNANT CATALOG (2015, background): “On a more macroscopic level, ECR,max can depend on the SNR hydrodynamics, namely the shock velocity and size, as well as on the ambient density (Lagage & Cesarsky 1983; Bell & Lucek 2001; Bell 2004; Ptuskin & Zirakashvili 2003, 2005; Blasi et al. 2007; Zirakashvili & Ptuskin 2008; Bell et al. 2013).”
NONTHERMAL RADIATION OF YOUNG SUPERNOVA REMNANTS: THE CASE OF RX J1713.7−3946 (2010, background): “However, similar to the case of the FS, the magnetic field can be significantly amplified also at the RS (see Ellison et al. 2005), for example, in the course of the non-resonant streaming instability introduced by Bell (2004).”
Cosmic-ray acceleration in supernova remnants: non-linear theory revised (2012, background): “18) which may play a relevant role, like for instance the excitation of Bell’s non-resonant modes [52, 53], or the development of large scales structures due to fire-hose instability [54, 55], which may be most effective where the CR distribution function is most anisotropic, i.”
On the role of injection in kinetic approaches to non‐linear particle acceleration at non‐relativistic shock waves (2005, background): “…which is still lacking in the calculations of the non-linear particle acceleration at shock waves, namely the possible amplification of the background magnetic field, found in the numerical simulations by Lucek & Bell (2000, 2000a) and Bell & Lucek (2001) and recently described by Bell (2004).”
Nonlinear Diffusive Shock Acceleration with Magnetic Field Amplification (2006, methodology): “…with B-Field Amplification Besides the limited results from PIC simulations, the only models of magnetic field generation with B3B0 in nonlinear DSA that we are aware of are the semianalytic results of Bell & Lucek (2001), Bell (2004, 2005), Ptuskin & Zirakashvili (2003), and Amato & Blasi (2006).”
Long-Term Evolution of Magnetic Turbulence in Relativistic Collisionless Shocks: Electron-Positron Plasmas (2007, background): “This is a relativistic version of Bell’s (1978) (also see Bell 2004, 2005) picture of particle acceleration in non-relativistic shocks.”
SIMULATIONS OF ION ACCELERATION AT NON-RELATIVISTIC SHOCKS. II. MAGNETIC FIELD AMPLIFICATION (2014, background): “However, there is a short-wavelength instability (the non-resonant hybrid, NRH, instability; Bell 2004, 2005) that is predicted to grow faster than the resonant one.”
Cosmic ray acceleration and escape from supernova remnants (2013, methodology): “Firstly, as shown by Bell (2004) the NRH instability is driven by the CR current density jCR. Higher order anisotropies do not directly contribute to the instability.”
Cosmic ray transport in the Galaxy: A review (2017, background): “As far as particles’ confinement in the accelerators is concerned, it was realised by Bell (2004) that a branch of this instability, that had not previously been considered, has an especially fast growth in the vicinity of a SNR shock and can in principle explain the large magnetic fields implied by”
Gamma-rays from molecular clouds illuminated by cosmic rays escaping from interacting supernova remnants (2010, methodology): “Although the magnetic field amplification around the shock is studied by the linear analysis (Bell 2004; Reville et al. 2007; Ohira et al. 2009b) and many numerical simulations (Lucek & Bell 2000; Giacalone & Jokipii 2007; Niemiec et al. 2008; Reville et al. 2008; Riquelme & Spitkovsky 2009; Inoue…”
Observational Signatures of Particle Acceleration in Supernova Remnants (2012, methodology): “Their are several means by which this magnetic field amplification occurs (see elsewhere in this volume), but a mechanism that received a lot of attention is the so-called Bell’s instability (Bell, 2004).”