On the spectrum of high-energy cosmic rays produced by supernova remnants in the presence of strong cosmic-ray streaming instability and wave dissipation

By V. Ptuskin, V. Zirakashvili. 2004

186 citations recorded by the source corpus.

The cosmic-ray streaming instability creates strong magnetohydrodynamic turbulence in the precursor of a SN shock. The level of turbulence determines the maximum energy of cosmic-ray particles accelerated by the diffusive shock accelera- tion mechanism. In this paper we present the continuation of previous work (Ptuskin & Zirakashvili 2003). We assume that Kolmogorov type nonlinear wave interactions together with ion-neutral collisions restrict the amplitude of the random mag- netic field. As a result, the maximum energy of the accelerated particles strongly depends on the age of a SNR. The average spectrum of cosmic rays injected in the interstellar medium in the course of the adiabatic SNR evolution (the Sedov stage) is approximately Q(p)p 2 ∝ p −2 at energies larger than 10−30 GeV/nucleon and with a maximum particle energy that is close to the position of the knee in the cosmic-ray spectrum observed at ∼4 × 10 15 eV. At an earlier stage of SNR evolution - the ejecta-dominated stage described by the Chevalier-Nadyozhin solution, the particles are accelerated to higher energies and have a rather steep power-law distribution. These results suggest that the knee may mark the transition from the ejecta-dominated to the adiabatic evolution of SNR shocks which accelerate cosmic rays.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/17da727c18aed729f9cd09610c05b639f4ce591e

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

Gamma-rays from molecular clouds illuminated by cosmic rays escaping from interacting supernova remnants (2010, methodology): “We assume the Bohm like diffusion coefficient D = D0p and ℓesc = κRsh as a geometrical confinement condition, where we adopt κ = 0.04 throughout the paper (Ptuskin & Zirakashvili 2005).”
SIMULATIONS OF ION ACCELERATION AT NON-RELATIVISTIC SHOCKS. I. ACCELERATION EFFICIENCY (2013, background): “…and the measured one can be explained by accounting for the CR transport in the Galaxy caprioli@astro.princeton.edu (the residence time is inferred to be a decreasing function of the energy) and for the differential escape from the sources (e.g., Ptuskin & Zirakashvili 2005; Caprioli et al. 2011).”
OBSERVATION OF SUPERNOVA REMNANT IC 443 WITH THE FERMI LARGE AREA TELESCOPE (2010, methodology): “The maximum energy depends on the condition of the acceleration site: Ptuskin & Zirakashvili (2005) have incorporated various instabilities into DSA and predict the maximum energy as a function of the SNR age.”
Observational Signatures of Particle Acceleration in Supernova Remnants (2012, background): “As CRs escape from remnants, they have a spectrum with a power-law index of approximately two (Ptuskin and Zirakashvili, 2005).”
Nonlinear Diffusive Shock Acceleration with Magnetic Field Amplification (2006, background): “An important attempt at describing turbulence with B/B3 1 was made by Ptuskin & Zirakashvili (2003, 2005).”
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).”
Broad-band non-thermal emission from molecular clouds illuminated by cosmic rays from nearby supernova remnants (2009, methodology): “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).”
Study of Nonthermal Emission from SNR RX J1713.7–3946 with Suzaku (2008, background): “…one should take into account that even in the case of effective acceleration the highest energy protons beyond 100 TeV escape the source in a quite short time scales, and hence do not contribute to the gamma-ray production at the present epoch (Ptuskin & Zirakashvili 2005; Gabici & Aharonian 2007).”
SPECTRUM OF GALACTIC COSMIC RAYS ACCELERATED IN SUPERNOVA REMNANTS (2010, background): “It can be shown, see e.g. Ptuskin & Zirakashvili (2005), that the transformation of supernova explosion energy to cosmic rays becomes efficient from the beginning of the Sedov stage of the shock evolution (i.e. when the mass of supernova ejecta becomes equal to the mass of swept-up gas) and…”