Limits on diffusive shock acceleration in supernova remnants in the presence of cosmic-ray streaming instability and wave dissipation

By V. Ptuskin, V. Zirakashvili. 2003

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The instability in the cosmic-ray precursor of a supernova shock moving in interstellar medium is studied. The level of magnetohydrodynamic turbulence in this region determines the maximum energy of particles accelerated by the diffusive shock acceleration mechanism. A high efficiency of cosmic ray acceleration is accepted, and the consideration is not limited by the case of weak turbulence. It is assumed that Kolmogorov-type nonlinear wave interactions together with the ion-neutral collisions restrict the amplitude of the random magnetic field. As a result, the maximum energy of accelerated particles strongly depends on the age of the supernova remnant. The maximum energy can be as high as ∼10 17 Z eV in young supernova remnants and falls to about ∼10 10 Z eV at the end of the Sedov stage. Thus the standard estimate of maximum particle energy based on the Bohm limit calculated for the interstellar magnetic field strength is not justified in this case. This finding may explain why supernova remnants with age of more than a few thousand years are not prominent sources of very high energy gamma-rays.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/af1dbec5369315d07823edc1ffd9d6a1e70d6c5e

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Citations in the corpus

Detection of Sub-TeV Gamma Rays from the Galactic Center Direction by CANGAROO-II (2004, result): “For example, the range of values is consistent with recent theoretical predictions for shock acceleration in supernova remnants (Ptuskin & Zirakashvili 2003).”
Cosmic-Ray Scattering and Streaming in Compressible Magnetohydrodynamic Turbulence (2004, background): “In this situation a di erent expression for the growth rate is applicable(Ptuskin & Zirakashvili2003): (k)’ ak U3 cVA( am ax (1+ a) 1 )(krg0)a(1+ A 2 tot)(1 a)=2 ; (16c) where isthe ratio ofthe pressure ofCRsatthe shock and the upstream m om entum ux entering the shock front,U is the shock front…”
On the spectrum of high-energy cosmic rays produced by supernova remnants in the presence of strong cosmic-ray streaming instability and wave dissipation (2004, background): “The acceleration of cosmic rays and their streaming instability in a wide range of shock veloc- ities was considered in our paper Ptuskin & Zirakashvili (2003) (Paper I).”
Nonlinear Diffusive Shock Acceleration with Magnetic Field Amplification (2006, methodology): “An important attempt at describing turbulence with B/B3 1 was made by Ptuskin & Zirakashvili (2003, 2005).”
FERMI LAT DISCOVERY OF EXTENDED GAMMA-RAY EMISSION IN THE DIRECTION OF SUPERNOVA REMNANT W51C (2009, methodology): “According to Ptuskin & Zirakashvili (2003), the maximum attainable momentum in the presence of wave dissipation by ion-neutral collisions is estimated as p max ( T 0 ) ∼ 30 ( n/ 1 cm − 3 ) − 1 / 2 GeV c − 1 , using the SNR parameters described above.”
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).”
Cosmic ray acceleration and escape from supernova remnants (2013, methodology): “…the spectra of CR at the shock during acceleration or that of CR carried downstream into the interior of the SNR. Related analyses based on different models of CR escape can be found in Caprioli et al (2010a), Drury (2011), Ohira et al (2010), Ptuskin & Zirakashvili (2003) and Ptuskin et al (2010).”
Superbubbles and energetic particles in the Galaxy. I. Collective effects of particle acceleration (2004, methodology): “…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 (3 × 1015 eV), but the ankle energy seems to remain…”
SPECTRUM OF GALACTIC COSMIC RAYS ACCELERATED IN SUPERNOVA REMNANTS (2010, background): “Although the maximum energy probably quickly decreases in the old remnants (see Ptuskin & Zirakashvili (2003)), we neglect this effect in our present calculations since it would require an introduction of an additional rather uncertain parameter.”
Cosmic ray transport in the Galaxy: A review (2017, methodology): “Recently, Recchia et al. (2016) proposed an iterative semi-analytical method to determine the wind structure, the CR spectrum and spatial distribution and to determine whether a CR induced wind may be launched in the first place, depending on the conditions at the base of the wind (Galactic rotation”
The Milky Way’s Kiloparsec-Scale Wind: A Hybrid Cosmic-Ray and Thermally Driven Outflow (2007, background): “…in the turbulent cascade seen in both experiments and theoretical studies of MHD turbulence (see, e.g. Shebalin et al. 1983; Goldreich & Sridhar 1995; Cho & Vishniac 2000; Milano et al. 2001), which has also been invoked in studies of turbulence in supernovae as well (Ptuskin & Zirakashvili 2003).”