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
收藏
页码：193 / 202
相关论文
共 50 条
  • [41] The supernova remnant W44: Confirmations and challenges for cosmic-ray acceleration
    Cardillo, M.
    Tavani, M.
    Giuliani, A.
    Yoshiike, S.
    Sano, H.
    Fukuda, T.
    Fukui, Y.
    Castelletti, G.
    Dubner, G.
    ASTRONOMY & ASTROPHYSICS, 2014, 565
  • [42] DIFFUSIVE COSMIC-RAY ACCELERATION AT RELATIVISTIC SHOCK WAVES WITH MAGNETOSTATIC TURBULENCE
    Schlickeiser, R.
    ASTROPHYSICAL JOURNAL, 2015, 809 (02):
  • [43] Cosmic ray transport in anisotropic magnetohydrodynamic turbulence - II. Shear Alfven waves
    Teufel, A
    Lerche, I
    Schlickeiser, R
    ASTRONOMY & ASTROPHYSICS, 2003, 397 (03) : 777 - 788
  • [44] DIRECT EVIDENCE FOR HADRONIC COSMIC-RAY ACCELERATION IN THE SUPERNOVA REMNANT IC 443
    Tavani, M.
    Giuliani, A.
    Chen, A. W.
    Argan, A.
    Barbiellini, G.
    Bulgarelli, A.
    Caraveo, P.
    Cattaneo, P. W.
    Cocco, V.
    Contessi, T.
    D'Ammando, F.
    Costa, E.
    De Paris, G.
    Del Monte, E.
    Di Cocco, G.
    Donnarumma, I.
    Evangelista, Y.
    Ferrari, A.
    Feroci, M.
    Fuschino, F.
    Galli, M.
    Gianotti, F.
    Labanti, C.
    Lapshov, I.
    Lazzarotto, F.
    Lipari, P.
    Longo, F.
    Marisaldi, M.
    Mastropietro, M.
    Mereghetti, S.
    Morelli, E.
    Moretti, E.
    Morselli, A.
    Pacciani, L.
    Pellizzoni, A.
    Perotti, F.
    Piano, G.
    Picozza, P.
    Pilia, M.
    Pucella, G.
    Prest, M.
    Rapisarda, M.
    Rappoldi, A.
    Scalise, E.
    Rubini, A.
    Sabatini, S.
    Striani, E.
    Soffitta, P.
    Trifoglio, M.
    Trois, A.
    ASTROPHYSICAL JOURNAL LETTERS, 2010, 710 (02) : L151 - L155
  • [45] Kinetic Simulations of Cosmic-Ray-modified Shocks. II. Particle Spectra
    Caprioli, Damiano
    Haggerty, Colby C.
    Blasi, Pasquale
    ASTROPHYSICAL JOURNAL, 2020, 905 (01):
  • [46] ASSESSING THE FEASIBILITY OF COSMIC-RAY ACCELERATION BY MAGNETIC TURBULENCE AT THE GALACTIC CENTER
    Fatuzzo, M.
    Melia, F.
    ASTROPHYSICAL JOURNAL, 2012, 750 (01):
  • [47] The cosmic-ray precursor of relativistic collisionless shocks: A missing link in gamma-ray burst afterglows
    Milosavljevic, Milos
    Nakar, Ehud
    ASTROPHYSICAL JOURNAL, 2006, 651 (02): : 979 - 984
  • [48] COMPARISON OF DISTRIBUTED ACCELERATION AND STANDARD MODELS OF COSMIC-RAY TRANSPORT
    LETAW, JR
    SILBERBERG, R
    TSAO, CH
    GALACTIC COSMIC RAY HEAVY IONS, 1994, 15 (01): : 65 - 68
  • [49] Constraints on cosmic-ray acceleration and transport from isotope observations
    Wiedenbeck, ME
    Binns, WR
    Christian, ER
    Cummings, AC
    George, JS
    Hink, PL
    Klarmann, J
    Leske, RA
    Lijowski, M
    Mewaldt, RA
    Stone, EC
    von Rosenvinge, TT
    Yanasak, NE
    ACCELERATION AND TRANSPORT OF ENERGETIC PARTICLES OBSERVED IN THE HELIOSPHERE, 2000, 528 : 363 - 370
  • [50] COSMIC-RAY ACCELERATION IN INHOMOGENEOUS MAGNETIC-FIELDS ABOUT RELATIVISTIC SHOCKS
    LUCEK, SG
    BELL, AR
    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 1994, 268 (02) : 581 - 594
12345