Cosmic ray acceleration to very high energy through the non-linear amplification by cosmic rays of the seed magnetic field

By A. Bell, S. Lucek. 2001

329 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/2dde7fa2c4ccf1aeefcaf9cf709bb5aed83a0ebd

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Citations in the corpus

Observational Signatures of Particle Acceleration in Supernova Remnants (2012, background): “Bell and Lucek (2001) calculated that CRs, as they stream up and down the shock front, can amplify the magnetic fields themselves by even an order of magnitude.”
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).”
The Astrophysics of Ultrahigh-Energy Cosmic Rays (2011, methodology): “A modification to the traditional SNR scenario, such as magnetic field amplification in SN shocks (Bell & Lucek 2001), or a different progenitors such as Wolf-Rayet star winds (Biermann & Cassinelli 1993), and trans-relativistic supernovae (Budnik et al. 2008) may explain the energy gap from PeV to…”
PARTICLE ACCELERATION IN RELATIVISTIC MAGNETIZED COLLISIONLESS ELECTRON–ION SHOCKS (2010, background): “Later on, the so-called Bell’s currentdriven instability develops (Bell & Lucek 2001; Bell 2004; Reville et al. 2006), and the shock results from nonlinear steepening of the circularly-polarized Alfvénic-type waves associated with the instability (see §3.2 for details).”
Magnetic Fields in Supernova Remnants and Pulsar-Wind Nebulae (2011, background): “The question of magnetic-field amplification is intimately connected with that of efficient particle acceleration through the proposals of Bell & Lucek (2001) and Bell (2004) that cosmic-ray driven instabilities can greatly increase the magnetic-field strength.”
Cosmic ray acceleration and escape from supernova remnants (2013, unknown): “…the SN progenitor. ρR2 is independent of radius in a steady wind, in which case the CR energy depends only on u2s and η according to equation (20) thus favouring CR acceleration in the very early stages of rapid expansion as previously suggested by Völk & Biermann (1988) and Bell & Lucek (2001).”
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).”
Limits on diffusive shock acceleration in supernova remnants in the presence of cosmic-ray streaming instability and wave dissipation (2003, background): “It does not work in young supernova remnants at the age t <∼ 3 × 103 yr when cosmic ray stream instability generates a strong random magnetic field δB > B0 that reduces particle diffusion (in agreement with Bell & Lucek 2001 results).”
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).”
Turbulent amplification of magnetic field and diffusive shock acceleration of cosmic rays (2004, methodology): “Bell & Lucek (2001) used an analytic model to estimate the way in which turbulent magnetic field amplification might extend the maximum CR energy, but the model was based upon hypothesized equations for the generation of magnetic field, which need substantiation (or amendment) if the results are to…”
Broad-band non-thermal emission from molecular clouds illuminated by cosmic rays from nearby supernova remnants (2009, background): “The value of pmax depends on a few crucial but poorly known aspects of the problem, including the nature of CR–driven instability operating in the shock precursor and the level of wave damping (Bell and Lucek 2001; Bell 2004; Ptuskin and Zirakashvili 2005; Blasi et al. 2007; Vladimirov et al. 2006).”
Non-linear particle acceleration at non-relativistic shock waves in the presence of self-generated turbulence (2006, background): “This problem is in fact even more serious for those approaches that predict levels of magnetic field amplification which are much higher than those found here (e.g. Bell & Lucek (2001); Bell (2004)).”
A Physical Relationship between Electron-Proton Temperature Equilibration and Mach Number in Fast Collisionless Shocks (2006, background): “Such a magnetic field amplification has already been proposed in the context of cosmic ray acceleration in shocks (Lucek & Bell 2000, Bell & Lucek 2001).”
Magnetic field amplification in Tycho and other shell-type supernova remnants (2004, background): “This extends earlier arguments put forward by Bell & Lucek (2001) who estimated the maximum achievable energy cpmax.”
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).”