Dissipation of Magnetohydrodynamic Waves on Energetic Particles: Impact on Interstellar Turbulence and Cosmic-Ray Transport

By V. Ptuskin, Igor V. Moskalenko, F. C. Jones, A. Strong, V. Zirakashvili. 2005

284 citations recorded by the source corpus.

The physical processes involved in diffusion of Galactic cosmic rays in the interstellar medium are addressed. We study the possibility that the nonlinear MHD cascade sets the power-law spectrum of turbulence that scatters charged energetic particles. We find that the dissipation of waves due to the resonant interaction with cosmic-ray particles may terminate the Kraichnan-type cascade below wavelengths 1013 cm. The effect of this wave dissipation has been incorporated in the GALPROP numerical propagation code in order to asses the impact on measurable astrophysical data. The energy dependence of the cosmic-ray diffusion coefficient found in the resulting self-consistent model may explain the peaks in the secondary to primary nuclei ratios observed at about 1 GeV nucleon-1.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/0575d3a62e5c0d113e5eb6981cebd4fded40ae52

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Citations in the corpus

The 511 keV emission from positron annihilation in the Galaxy (2010, background): “The derived propagation parameters (timescale of CR confinement, diffusion coefficient, etc.) are model dependent and can vary significantly (e.g., Ptuskin et al., 2006).”
Inverse Compton Origin of the Hard X-Ray and Soft Gamma-Ray Emission from the Galactic Ridge (2008, methodology): “We give a very brief summary of GALPROP; for details we refer the reader to the relevant papers (Moskalenko & Strong 1998, 2000; Moskalenko et al. 2002; Ptuskin et al. 2006; Strong & Moskalenko 1998; Strong et al. 2000, 2004b) and the dedicated website3.”
The Fermi Galactic Center GeV Excess and Implications for Dark Matter (2017, methodology): “…we will model Galactic interstellar emission from the large-scale CR populations in the Galaxy starting from predictions obtained through the GALPROP code71 (Moskalenko & Strong 1998; Strong et al. 2000, 2004; Ptuskin et al. 2006; Strong et al. 2007; Porter et al. 2008; Vladimirov et al. 2011).”
GeV OBSERVATIONS OF STAR-FORMING GALAXIES WITH THE FERMI LARGE AREA TELESCOPE (2012, unknown): “The diffusive escape timescale can be estimated asτdif ∼ z2h/6D∼ (1−2)×107 yr for a halo height ofzh = 4 kpc, and taking diffusion coefficients in the rangeD = (4− 8)×1028 cm2 s−1 for a particle rigidity of ∼10 GV (Ptuskin et al. 2006).”
The interstellar cosmic-ray electron spectrum from synchrotron radiation and direct measurements. (2011, background): “A54, page 7 of 13 is in fact similar to that in the wave-damping model of Ptuskin et al. (2006) and hence has also a plausible physical basis.”
The Nine Lives of Cosmic Rays in Galaxies (2015, methodology): “On the other hand, diffusion models without reacceleration have a problem to reproduce the B/C spectrum without either a very large break in Dxx(p) (Strong & Moskalenko 1998), an additional velocity dependence in Dxx(p), or dissipation of MHD waves (Ptuskin et al. 2006).”
CONSTRAINTS ON COSMIC-RAY PROPAGATION MODELS FROM A GLOBAL BAYESIAN ANALYSIS (2010, methodology): “…with Our Previous Results In general, there is remarkable agreement between the “byeye” fitting in the past (e.g., Strong & Moskalenko 1998, 2001; Moskalenko et al. 2002; Ptuskin et al. 2006) and the parameter constraints found using the refined Bayesian inference analysis described in this paper.”
Cosmic ray driven outflows in global galaxy disc models (2013, result): “Our fiducial choice of diffusion parameter κCR is consistent both with recent GALPROP models (e.g. Ptuskin et al. 2006; Ackermann et al. 2012) and with observational measurements (e.g. Strong & Moskalenko 1998; Tabatabaei et al. 2013).”
SPECTRUM OF GALACTIC COSMIC RAYS ACCELERATED IN SUPERNOVA REMNANTS (2010, background): “Fluctuations of cosmic ray intensity and anisotropy were addressed in particular by Erlykin & Wolfendale (2006); Ptuskin et al. (2006a).”
THE SPECTRUM AND MORPHOLOGY OF THE FERMI BUBBLES (2014, methodology): “In Section 3, we model the Galactic foreground emission components by using maps generated with the GALPROP1 (Moskalenko & Strong 1998; Strong et al. 2000, 2004; Ptuskin et al. 2006; Strong et al. 2007; Porter et al. 2008; Vladimirov et al. 2011) CR propagation and interactions code as templates.”
Cosmic-ray propagation with DRAGON2: I. numerical solver and astrophysical ingredients (2016, background): “We study the propagation of CRs in the -5 kpc ≤ z ≤ 5 kpc region for three different setups of the binning along the z-axis: – 24 – • An EB with nz = 501, corresponding to a constant resolution of 20 pc. • A NEB with nz = 31, where the bins width is 20 pc for |z| ≤ 100 pc and then grows to 50 pc, 10”
Solar Modulation of Cosmic Rays (2013, background): “For energies below ∼ 10 GeV, which is of great interest to solar modulation studies, the galactic propagation processes are acknowledged as less precise as illustrated comprehensively by Ptuskin et al. (2006) and Webber and Higbie (2008, 2009).”
A Markov Chain Monte Carlo technique to sample transport and source parameters of Galactic cosmic rays - II. Results for the diffusion model combining B/C and radioactive nuclei (2010, background): “…parameters, because their value can be compared to theoretical predictions for the transport in turbulent magnetic fields (e.g., Casse et al. 2002; Ptuskin et al. 2006; Minnie et al. 2007; Tautz et al. 2008, Yan & Lazarian 2008 and references therein), or related to the source spectra predicted…”