Cosmic Ray Astrophysics

By R. Schlickeiser. 2002

667 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/3227b4ba46516b3a8008d9abfbf2974be1870802

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Citations in the corpus

Acceleration of primary and secondary particles in galaxy clusters by compressible MHD turbulence: from radio haloes to gamma-rays (2010, background): “Schlickeiser & Miller 1998; Brunetti & Lazarian 2007; Yan, Lazarian & Petrosian 2008) being stronger for θ ∼ π/2 and causing the spectrum of the turbulent modes to become anisotropic at scales k ∼ kc(θ ). On the other hand, in Brunetti & Lazarian (2007) we have shown that, under physical conditions ”
Cosmic ray transport in galaxy clusters: implications for radio halos, gamma-ray signatures, and cool core heating (2010, background): “In our own Galaxy, the ratio of the spectral energy flux of CRp to CRe between 1. . . 10 GeV is about one hundred (Schlickeiser 2002).”
Dust Dynamics in Compressible Magnetohydrodynamic Turbulence (2004, methodology): “For isotropic turbulence,the tensor ofthe form / E k( ij kikj=k2) was obtained to satisfy the divergence free condition k B = 0 (see Schlickeiser2002).”
Antinuclei in heavy-ion collisions (2018, background): “hypothesis. Another focus in the cosmic ray physics community is the investigation of the spectrum of positrons in space, which has connections to bulk primordial antimatter or dark matter hypotheses [59, 79, 81, 82, 83]. See Section 6.1 for further details. A variety of extensions beyond the Standa”
Cosmic ray feedback in hydrodynamical simulations of galaxy formation (2006, methodology): “We fix the overall strength by alluding to measurements in our own Galaxy (Berezinskii et al., 1990; Schlickeiser, 2002), which estimate a diffusivity along the magnetic field lines in the interstellar medium of approximately κISM ≈ 3× 1027 cm2 s ≈ 10 kpc 2 Gyr (53) Adopting our typical temperature ”
SEARCH FOR COSMIC-RAY-INDUCED GAMMA-RAY EMISSION IN GALAXY CLUSTERS (2013, neutral): “Second, ζe/ζp ∼ 1 is inconsistent with the observed ratio for Galactic CRs, which has a differential energy ratio of Ke/p ≃ 0.01 at 10 GeV (Schlickeiser 2002) and observations of supernova remnants constrain the ratio ζe/ζp ∼ 0.001 (Edmon et al. 2011; Morlino & Caprioli 2012).”
Magnetic Fields in Starburst Galaxies and the Origin of the FIR-Radio Correlation (2006, background): “The timescale for cosmic-ray protons to lose their energy to pion production is tpion 108 (n/1 cm 3) 1 yr (e.g., Schlickeiser 2002).”
THE PHYSICS OF THE FAR-INFRARED–RADIO CORRELATION. I. CALORIMETRY, CONSPIRACY, AND IMPLICATIONS (2009, background): “Since the CRs are inferred to travel through material of density neff ≈ 0.2 − 0.5 cm−3 (e.g., Connell 1998; Schlickeiser 2002), this implies that f ≈ 1.”
ANISOTROPIC THREE-DIMENSIONAL FOCUSED TRANSPORT OF SOLAR ENERGETIC PARTICLES IN THE INNER HELIOSPHERE (2010, background): “Higher order terms in Vsw/v have been neglected in Equation (2), and the variables are written in mixed reference frames, with the spatial coordinates in a fixed frame, and particle momentum and pitch angle in the solar wind frame(e.g., Ruffolo 1995; Schlickeiser 2002).”
PROPAGATION OF SOLAR ENERGETIC PARTICLES IN THREE-DIMENSIONAL INTERPLANETARY MAGNETIC FIELDS (2009, background): “Normally, there should be 10 independent Fokker–Planck diffusion coefficients (e.g., No. 1, 2009 PROPAGATION OF SOLAR ENERGETIC PARTICLES 111 Schlickeiser 2002; Zhang 2006).”
Cosmic-Ray Propagation: Nonlinear Diffusion Parallel and Perpendicular to Mean Magnetic Field (2007, methodology): “Astrophysical magnetic fields are turbulent and, therefore, the resonant and non-resonant (e.g., transient time damping, or TTD) interaction of cosmic rays with MHD turbulence is the accepted principal mechanism to scatter and isotropize cosmic rays (see Schlickeiser 2002).”
Constraining the population of cosmic ray protons in cooling flow clusters with γ-ray and radio observations: Are radio mini-halos of hadronic origin? (2003, methodology): “by Jaffe (1977), and reconsidered by Schlickeiser et al. (1987), and lately by Ohno et al. (2002). These acceleration processes of CRe possibly yield extended radio halos centered on the cluster (Brunetti et al. 2001) while there ar e also suggestions that radio mini-halos within a cooling flow clus”
Stochastic Acceleration of Electrons and Protons. I. Acceleration by Parallel-Propagating Waves (2004, background): “Thepositiveand negativefrequenciesm ean thatthe waves are right-and left-handed polarized,respectively,where the polarization is de ned relative to the large scale m agnetic eld (Schlickeiser 2002).”
The Starburst Contribution to the Extragalactic γ-Ray Background (2006, background): “Although this efficiency of cosmic ray production is reasonably consistent with the energetics of galactic cosmic rays (e.g., Schlickeiser 2002) and with the -ray luminosity of the Milky Way (Hunter et al. 1997; Strong et al. 2000), some models of nonlinear diffusive shock acceleration imply 0:5…”
Cosmic-Ray Scattering and Streaming in Compressible Magnetohydrodynamic Turbulence (2004, background): “This eld is turbulent and therefore,the resonant interaction ofcosm ic rays with M HD turbulencehasbeen discussed by m any authorsastheprincipalm echanism to scatter and isotropize cosm ic rays (Schlickeiser 2002).”
On the Momentum Diffusion of Radiating Ultrarelativistic Electrons in a Turbulent Magnetic Field (2008, methodology): “This is consistent with the appropriate Green’s function found by Schlickeiser et al. (1987) who, in a framework of the ‘hard-sphere’ approximation q = 2, considered also synchrotron emission and particle escape in addition to the bremsstrahlung radiation.”