Non-Linear Amplification of a Magnetic Field Driven by Cosmic Ray Streaming

By S. Lucek, A. Bell. 2000

300 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/0593e04f3f16c996771f476de9d074b52ec2f167

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Citations in the corpus

On the Magnetic Fields and Particle Acceleration in Cassiopeia A (2002, background): “9 field strength in the medium surrounding Cas A, possibly as the result of the stellar wind of the progenitor (Biermann & Cassinelli 1993), or it means that the magnetic field is being rapidly enhanced near the shock front (Lucek & Bell 2000).”
Cosmic ray acceleration and escape from supernova remnants (2013, methodology): “The MHD part of the code is the same as that used by Lucek & Bell (2000) and Bell (2004).”
TOWARD UNDERSTANDING THE COSMIC-RAY ACCELERATION AT YOUNG SUPERNOVA REMNANTS INTERACTING WITH INTERSTELLAR CLOUDS: POSSIBLE APPLICATIONS TO RX J1713.7−3946 (2011, background): “…region far from the primary shock front suggesting that other possible amplification mechanisms such as the cosmic-ray streaming instability (Lucek & Bell 2000) and/or dynamo effect driven by the interaction between cosmic-ray precursor and density fluctuation (Beresnyak et al. 2009) might…”
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).”
Cosmic-ray energy spectrum and composition up to the ankle - the case for a second Galactic component (2016, background): “However, numerical simulations have shown that the magnetic field near supernova shocks can be amplified considerably up to ⇠10 100 times the mean interstellar value (Lucek & Bell 2000; Reville & Bell 2012).”
Observational Signatures of Particle Acceleration in Supernova Remnants (2012, background): “In the precursor region, magnetic-field amplification (Lucek and Bell, 2000; Bell, 2004; Ohira and Takahara, 2010; Bykov et al., 2011b; Schure and Bell, 2011; Reville and Bell, 2011) and plasma heating (McKenzie and Völk, 1982; Ghavamian et al., 2007; Rakowski et al., 2008; Niemiec et al., 2008;…”
The origin of galactic cosmic rays (2013, unknown): “On the other hand, the non-resonant mode first discussed by Bell (2004) (but see also (Lucek and Bell, 2000; Bell and Lucek, 2001)) has a growth rate which can be much larger than any other unstable mode, and can certainly lead to large magnetic fields at the shock.”
The Astrophysics of Ultrahigh-Energy Cosmic Rays (2011, unknown): “More detailed work was conducted by, e.g., McKenzie & Voelk (1982); Berezhko & Ellison (1999); Lucek & Bell (2000); Malkov & O’C Drury (2001); Bell & Lucek (2001); Bell (2004); Amato & Blasi (2005, 2006, 2009); Zirakashvili et al. (2008); Reville et al. (2008).”
Interpretation of AMS-02 electrons and positrons data (2014, methodology): “Moreover, fixing a typical magnetic field of B = 30μG (adopted in the following of our analysis) [45, 50, 52–58], and employing Eq.”
Superbubbles and energetic particles in the Galaxy. I. Collective effects of particle acceleration (2004, background): “…be noted, in particular, that allowing for large fluctuations of the magnetic field around the SN shock (up to 100 times the ambient field or more; Lucek & Bell 2000; Bell & Luceck 2001; Berezhko et al. 2003; Ptuskin & Zirakashvili 2003) does help to reach energies around or even above the knee…”
Limits on diffusive shock acceleration in supernova remnants in the presence of cosmic-ray streaming instability and wave dissipation (2003, background): “Analyzing the early stage of supernova remnant evolution when the shock velocity is high, ush ∼ 104 km s−1, Lucek & Bell (2000), Bell & Lucek (2001) found that the cosmic ray streaming instability can be so strong that the amplified field δB >∼ 10−4 G far exceeds the magnetic field in the…”
Teraelectronvolt Astronomy (2010, background): “Both resonant and non-resonant instabilities of the magnetic field are driven by CR currents (Lucek & Bell (2000), see Caprioli et al. (2008) for further references).”
A Spatial and Spectral Study of Nonthermal Filaments in Historical Supernova Remnants: Observational Results with Chandra (2004, methodology): “Thetim eevolution oftheenergy density ofaccelerated protons (up)m ay also bediscussed from therelationsby Lucek & Bell(2000)as up = vs vA uB / B dvs / tage 1:2 ; (6) where vA B = p 4 and are the Alfv en velocity and the uid density,suggesting that accelerated protons in an SNR evolve with the sam e…”