Turbulence and particle acceleration in collisionless supernovae remnant shocks II. Cosmic-ray transport

被引：0

作者：

Marcowith, A. ^{[1
]}

Lemoine, M. ^{[2
]}

Pelletier, G. ^{[3
,4
]}

机构：

[1] Centre d'Études Spatiales et du Rayonnement, CNRS, Université Paul Sabatier Toulouse 3, 9 avenue du Colonel Roche, 031028 Toulouse Cedex, France

[2] Institut d'Astrophysique de Paris, UMR 7095 CNRS, Université Pierre and Marie Curie, 98bis boulevard Arago, 75014 Paris, France

[3] Laboratoire d'Astrophysique de Grenoble, CNRS, Université Joseph Fourier II, BP 53, 38041 Grenoble

[4] Institut Universitaire de France, France

来源：

Astronomy and Astrophysics | 1600年 / 453卷 / 01期

关键词：

Supernovae remnant shock waves could be at the origin of cosmic rays up to energies in excess of the knee (E 3 × 1015 eV) if the magnetic field is efficiently amplified by the streaming of accelerated particles in the shock precursor. This paper follows up on a previous paper (Pelletier et al. 2006; A&A; in press) which derived the properties of the MHD turbulence so generated; in particular its anisotropic character; its amplitude and its spectrum. In the present paper; we calculate the diffusion coefficients; also accounting for compression through the shock; and show that the predicted three- dimensional turbulence spectrum k⊥S 3d(k; k⊥; ∝; k; -1; k⊥-α(with k and k⊥ the wavenumber components along and perpendicular to the shock normal) generally leads to Bohm diffusion in the parallel direction. However; if the anisotropy is constrained by a relation of the form k ∝ k⊥2/3; which arises when the turbulent energy cascade occurs at a constant rate independent of scale; then the diffusion coefficient loses its Bohm scaling and scales as in isotropic Kolmogorov turbulence. We show that these diffusion coefficients allow to account for X-ray observations of supernova remnants. This paper also calculates the modification of the Fermi cycle due to the energy lost by cosmic rays in generating upstream turbulence and the concomittant steepening of the energy spectrum. Finally we confirm that cosmic rays can produced an amplified turbulence in young SNr during their free expansion phase such that the maximal energy is close to the knee and the spectral index is close to 2.3 in the warm phase of the interstellar medium. © ESO 2006;

D O I：

暂无

中图分类号：

学科分类号：

摘要：

Journal article (JA)

引用

页码：193 / 202

共 50 条

[21] Particle acceleration and turbulence in cosmic ray shocks: possible pathways beyond the Bohm limit
Malkov, M. A.
Diamond, P. H.
TURBULENCE AND NONLINEAR PROCESSES IN ASTROPHYSICAL PLASMAS, 2007, 932 : 290 - +
[22] Particle acceleration and cosmic-ray origin in the galaxy
Tanimori, T
SCIENCE OF SUPERSTRONG FIELD INTERACTIONS, 2002, 634 : 161 - 168
[23] COSMIC-RAY ACCELERATION BY LONG-WAVE TURBULENCE
PTUSKIN, VS
SOVIET ASTRONOMY LETTERS, 1988, 14 (04): : 255 - 257
[24] Cosmic-Ray Acceleration from Turbulence in Molecular Clouds
Gaches, Brandt A. L.
Walch, Stefanie
Lazarian, A.
ASTROPHYSICAL JOURNAL LETTERS, 2021, 917 (02)
[25] Molecular Clouds as a Probe of Cosmic-Ray Acceleration in a Supernova Remnant
Fujita, Yutaka
Ohira, Yutaka
Tanaka, Shuta J.
Takahara, Fumio
10TH INTERNATIONAL SYMPOSIUM ON ORIGIN OF MATTER AND EVOLUTION OF GALAXIES, 2010, 1269 : 126 - 130
[26] MOLECULAR CLOUDS AS A PROBE OF COSMIC-RAY ACCELERATION IN A SUPERNOVA REMNANT
Fujita, Yutaka
Ohira, Yutaka
Tanaka, Shuta J.
Takahara, Fumio
ASTROPHYSICAL JOURNAL LETTERS, 2009, 707 (02): : L179 - L183
[27] The Effect of Intermittent Turbulence on Cosmic-ray Transport
le Roux, J. A.
PARTIALLY IONIZED PLASMAS THROUGHOUT THE COSMOS - PROCEEDINGS OF THE 2010 HUNTSVILLE WORKSHOP, 2011, 1366
[28] RAPID COSMIC-RAY ACCELERATION AT PERPENDICULAR SHOCKS IN SUPERNOVA REMNANTS
Takamoto, Makoto
Kirk, John G.
ASTROPHYSICAL JOURNAL, 2015, 809 (01):
[29] COSMIC-RAY ACCELERATION DURING THE IMPACT OF SHOCKS ON DENSE CLOUDS
JONES, TW
KANG, H
ASTROPHYSICAL JOURNAL, 1993, 402 (02): : 560 - 573
[30] Cosmic-ray acceleration and gamma-ray signals from radio supernovae
Marcowith, A.
Renaud, M.
Dwarkadas, V.
Tatischeff, V.
NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS, 2014, 256 : 94 - 100

← 1 2 3 4 5 →