The Modified Weighted Slab Technique: Models and Results

By F. C. Jones, A. Lukasiak, V. Ptuskin, W. Webber. 2000

143 citations recorded by the source corpus.

In an attempt to understand the source and propagation of Galactic cosmic rays, we have employed the modified weighted slab technique along with recent values of the relevant cross sections to compute primary to secondary ratios including B/C and sub-Fe/Fe for different Galactic propagation models. The models that we have considered are the disk-halo diffusion model, the dynamical halo wind model, the turbulent diffusion model, and a model with minimal reacceleration. The modified weighted slab technique will be briefly discussed and a more detailed description of the models will be given. We will also discuss the impact that the various models have on the problem of anisotropy at high energy and discuss what properties of a particular model bear on this issue.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/e5e61bbe0d76fa4097f366b593834d75621c0e06

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Citations in the corpus

Dissipation of Magnetohydrodynamic Waves on Energetic Particles: Impact on Interstellar Turbulence and Cosmic-Ray Transport (2005, background): “A major problem of concern for diffusion on a Kraichnan spectrum is the relatively strong dependence of diffusion on energy which leads to an unacceptably large anisotropy of cosmic rays especially above 1014 eV, see Jones et al. (2001), Ptuskin et al. (2003b).”
SPECTRUM OF GALACTIC COSMIC RAYS ACCELERATED IN SUPERNOVA REMNANTS (2010, methodology): “Based on the paper Jones et al. (2001), we choose the escape length in the form Xe = 11.8 (v/c) (p/4.9ZGV) −0.54 g/cm2 (7) at p/Z ≥ 4.9 GV; and Xe ∝ v/c at p/Z < 4.9 GV. Eq.”
CALIBRATING EXTINCTION-FREE STAR FORMATION RATE DIAGNOSTICS WITH 33 GHz FREE–FREE EMISSION IN NGC 6946 (2011, methodology): “…the propagation of CR electrons is described by a random walk with an energydependent diffusion coefficient DE (e.g., Ginzburg et al. 1980), where DE = 5 × 10 28 cm2 s−1 for E < 1 GeV and 5 × 1028(E/GeV)1/2 cm2 s−1 for E ≥ 1 GeV (e.g., Jones et al. 2001; Moskalenko et al. 2002; Maurin et al. 2002).”
Interstellar Turbulence II: Implications and Effects (2004, background): “…scatter so frequently that their flux at the Earth is isotropic to within 5 × 10−4 (Cutler & Groom 1991, Munakata et al. 1997), even though there are only a handful of nearby sources (i.e., Geminga, Vela, Lupus Loop, Loop III—see Ptuskin & Soutoul 1998, Jones et al. 2001, Taillet & Maurin 2003).”
Cosmic Rays below Z = 30 in a Diffusion Model: New Constraints on Propagation Parameters (2001, background): “A more fundamental origin may be found for the previous expression, as one can show in a one-dimensional di†usion model with convection (Jones et al. 2001).”
The H.E.S.S. Survey of the Inner Galaxy in Very High Energy Gamma Rays (2005, methodology): “The distribution exhibits a mean of 2.32, marginally consistent with predictions by models of shock wave acceleration in SNRs (see, e.g., Berezhko & Völk 1997, 2000) and as expected for the source spectrumofGalactic cosmic rays (see, e.g., Jones et al. 2001).”
A database of charged cosmic rays (2013, methodology): “The CR data are the backbone of Galactic CR propagation studies (e.g., Jones et al. 2001; Maurin et al. 2001; Strong et al. 2007; Evoli et al. 2008).”
Cosmic-ray energy spectrum and composition up to the ankle - the case for a second Galactic component (2016, background): “The e↵ect of Galactic winds on the transport of cosmic rays in the Galaxy has been discussed quite extensively (Lerche & Schlickeiser 1982a; Bloemen et al. 1993; Strong & Moskalenko 1998; Jones et al. 2001; Breitschwerdt et al. 2002).”
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): “At the same time, the assumption that the constant fraction ξcr of incoming gas momentum flux goes to the cosmic ray pressure at the shock, and the fact that the supernova remnant evolution is adiabatic lead to the average on ensemble of SNRs source spectrum of ultrarelativistic particles that is cl”
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, methodology): “Several diffusion models are considered in the literature (Webber et al. 1992; Bloemen et al. 1993; Strong & Moskalenko 1998; Jones et al. 2001; Maurin et al. 2001; Berezhko et al. 2003; Shibata et al. 2006; Evoli et al. 2008; Farahat et al. 2008).”
The Most Likely Sources of High-Energy Cosmic-Ray Electrons in Supernova Remnants (2003, background): “…it has been argued that the increase of the diffusion coefficient with energy should become slower than δ = 0.6 at somewhere beyond tens of GeV, and also that δ = 0.3 is plausible from a Kolmogorov-type spectrum of turbulence in the interstellar medium (e.g. Gaisser 1990, 2000; Jones et al. 2001).”
Limits on diffusive shock acceleration in supernova remnants in the presence of cosmic-ray streaming instability and wave dissipation (2003, background): “3m cm2 s−1, where β = v/c is the dimensionless particle velocity and Rm = pc/Z is the particle magnetic rigidity in units GV, see Jones et al. (2001), and thus the necessary condition of acceleration cannot be fulfilled for relativistic particles unless their diffusion coefficient is anomalously…”
GeV OBSERVATIONS OF STAR-FORMING GALAXIES WITH THE FERMI LARGE AREA TELESCOPE (2012, unknown): “The mean escape length for CR nuclei in the Milky Way isx̄ = τres mp 〈neff〉 c ≈ 12 g cm−2 (Jones et al. 2001) (cf. the interaction length is∼55 g cm−2).”