Non-linear particle acceleration at non-relativistic shock waves in the presence of self-generated turbulence

By E. Amato, P. Blasi. 2006

150 citations recorded by the source corpus.

Particle acceleration at astrophysical shocks may be very efficient if magnetic scattering is self-generated by the same particles. This non-linear process adds to the non-linear modification of the shock due to the dynamical reaction of the accelerated particles on the shock. Building on a previous general solution of the problem of particle acceleration with arbitrary diffusion coefficients, we present here the first semi-analytical calculation of particle acceleration with both effects taken into account at the same time; charged particles are accelerated in the background of Alfven waves that they generate due to the streaming instability, and modify the dynamics of the plasma in the shock vicinity.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/3d5c341997b3b0ac84e7f2517aa814babe123462

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In Astronomy and Astrophysics

1. A. Spitkovsky
2. D. Caprioli
3. L. Sironi
4. J. Vink
5. G. Morlino
6. F. Aharonian
7. A. Bykov
8. V. Zirakashvili

In Nuclear and High Energy Physics

1. A. Spitkovsky
2. D. Caprioli
3. L. Sironi
4. J. Vink
5. G. Morlino
6. F. Aharonian
7. A. Bykov
8. V. Zirakashvili

Citations in the corpus

• 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).”
• Cosmic-ray acceleration in supernova remnants: non-linear theory revised (2012, background): “[44, 46], in its extended version including particle escape from an upstream boundary [45] and the dynamical feedback of self-generated magnetic fields [28, 47].”
• Observational Signatures of Particle Acceleration in Supernova Remnants (2012, background): “…mechanisms due to CR instabilities in nonlinear diffusive shock acceleration were proposed recently by several studies Bell (2004, 2005); Amato and Blasi (2006); Vladimirov et al. (2006); Marcowith et al. (2006); Vladimirov et al. (2009); Zirakashvili and Ptuskin (2008); Bykov et al.…”
• SIMULATIONS OF ION ACCELERATION AT NON-RELATIVISTIC SHOCKS. II. MAGNETIC FIELD AMPLIFICATION (2014, methodology): “…for Alfvénic modes generated via resonant streaming instability for a shock weakly modified by the CR presence (see, e.g., Lagage & Cesarsky 1983; Amato & Blasi 2006, as well as Section 4.1), one gets: Pw(x) Pcr(x) M̃A ; Pw(x) = B 2 ⊥ 8π , (1) where Pw and Pcr are the magnetic and CR pressures,…”
• Shock waves in Eulerian cosmological simulations: main properties and acceleration of cosmic rays (2008, unknown): “…rely on the theory of nonlinear shock acceleration, which describes the acceleration of CR in shocks whose structure is modified by the back-reaction of CR energy (e.g. Ellison, Baring & Jones 1995; Malkov 1997; Blasi 2002, 2004a; Kang, Jones & Gieseler 2002; Kang & Jones 2005; Amato & Blasi 2006).”
• Nonlinear Diffusive Shock Acceleration with Magnetic Field Amplification (2006, methodology): “This choice of VG provides a lower limit on the amplification rate and was used in Amato & Blasi (2006).”
• The origin of galactic cosmic rays (2013, unknown): “Such a theory should also be able to describe the generation of magnetic field in the shock region as due to CR-driven instabilities (Amato and Blasi 2006; Caprioli et al. 2008, 2009b), although many problems still need to be solved.”
• PARTICLE ACCELERATION IN RELATIVISTIC MAGNETIZED COLLISIONLESS ELECTRON–ION SHOCKS (2010, background): “At late times (e.g., ωpit = 5062), the tail does not resemble a simple power-law with constant slope, but it seems to be somewhat concave, which may be due to the modification of the shock by accelerated ions (see §3.2), as discussed for non-relativistic shocks in SNRs by Amato & Blasi (2005, 2006).”
• Strong evidence for hadron acceleration in Tycho’s supernova remnant (2011, methodology): “The dot-dashed line shows the electron temperature computed including the heating due to Coulomb collisions. references therein (especially Amato & Blasi (2005, 2006)), which solves self-consistently the equations for conservation of mass, momentum and energy along with the diffusionconvection…”
• SIMULATIONS OF ION ACCELERATION AT NON-RELATIVISTIC SHOCKS. I. ACCELERATION EFFICIENCY (2013, methodology): “However, if some amplified magnetic modes were dissipated, for instance because of non-linear Landau damping, there should be an additional source of heating, usually referred to as turbulent (or Alfvén) heating (see, e.g., McKenzie & Völk 1982; Berezhko & Ellison 1999; Amato & Blasi 2006).”
• EFFICIENT COSMIC RAY ACCELERATION, HYDRODYNAMICS, AND SELF-CONSISTENT THERMAL X-RAY EMISSION APPLIED TO SUPERNOVA REMNANT RX J1713.7–3946 (2010, methodology): “We determine Emax p by limiting the 3 The model of nonlinear DSA we use here is based on the semianalytic model developed by Blasi, Gabici & Vannoni (2005) and Amato & Blasi (2006).”
• NONTHERMAL RADIATION OF YOUNG SUPERNOVA REMNANTS: THE CASE OF RX J1713.7−3946 (2010, background): “The characteristic diffusive scale of highest energy particles is a small fraction ξ0 1 of the shock radius (see Zirakashvili & Ptuskin 2008) and is determined by the generation and transport of MHD turbulence in the upstream region (see also Vladimirov et al. 2006; Amato & Blasi 2006).”