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  • 1
    Series available for loan
    Series available for loan
    Nonlinear perturbation theory for cosmic ray propagation in random magnetic fields (1973)
    Garching bei München
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    Call number: SR 90.1026(87)
    In: MPE-Report
    Type of Medium: Series available for loan
    Pages: 35 S.
    Series Statement: Max-Planck-Institut für Physik und Astrophysik, Institut für Extraterrestrische Physik 87
    Language: English
    Location: Magazine - must be ordered
    Branch Library: GFZ Library
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  • 2
    Series available for loan
    Series available for loan
    Spatial dependence of the pitch-angle and associated spatial diffusion coefficients for cosmic rays in interplanetary space (1973)
    Garching bei München
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    Call number: SR 90.1026(88)
    In: MPE-Report
    Type of Medium: Series available for loan
    Pages: 48 S.
    Series Statement: Max-Planck-Institut für Physik und Astrophysik, Institut für Extraterrestrische Physik 88
    Language: English
    Location: Magazine - must be ordered
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  • 3
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    Motions of the bow shock induced by interplanetary disturbances (1973)
    Garching bei München
    Associated volumes
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    Call number: SR 90.1026(85)
    In: MPE-Report
    Type of Medium: Series available for loan
    Pages: 32 S.
    Series Statement: Max-Planck-Institut für Physik und Astrophysik, Institut für Extraterrestrische Physik 85
    Language: English
    Location: Magazine - must be ordered
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  • 4
    Electronic Resource
    Electronic Resource
    Damping and nonlinear wave-particle interactions of Alfvén-waves in the solar wind (1973)
    Springer
    Astrophysics and space science 24 (1973), S. 31-49 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Since most Alfvén-waves in the solar wind are observed to come from the Sun, nonlinear wave-particle interactions can be expected to constitute their dominant dissipation process. The growth or damping of two circularly-polarized Alfvén-waves with wave vectors parallel to the ambient magnetic field is calculated using kinetic theory. If the waves are oppositely polarized they both damp proportional to their frequency. If the waves are of the same polarization, both the lower frequency wave and the plasma particles gain energy at the expense of the higher frequency wave. Thus, with increasing distance from the Sun, a steepening of the power spectrum is expected. For waves propagating in the same direction, the interaction is negligible for small β, while it becomes appreciable for β≥10−1. For conditions typical of the solar wind near 1 AU an observed half-hour linearly-polarized wave, for example, with δB=0(B 0) has a damping time of about 10 h.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00648673
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  • 5
    Electronic Resource
    Electronic Resource
    Nonlinear perturbation theory for cosmic ray propagation in random magnetic fields (1973)
    Springer
    Astrophysics and space science 25 (1973), S. 471-490 
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    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract A nonlinear perturbation theory is applied to the problem of pitch angle diffusion of energetic particles in random magnetic fields. To keep the analysis simple, the discussion is restricted to fluctuation fields, consisting of Alfvén waves. It is shown that the failure of quasilinear theory at small particle velocities parallel to the average field can be overcome by a statistically exact treatment of the particle orbits in the first order fields. In fact, for spherical power spectra which, in addition, do not fall off too steeply with increasing frequency, the conventional perturbation theory also leads to formally convergent expressions for the scattering mean free path. These results are shown to be quite satisfactory, even in a quantitative sense. For more general physically realistic power spectra, however, a divergence-free diffusion theory is indispensible. A simple representation for the resulting pitch-angle diffusion coefficient is suggested.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00649186
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  • 6
    Electronic Resource
    Electronic Resource
    Spatial dependence of the pitch-angle and associated spatial diffusion coefficients for cosmic rays in interplanetary space (1974)
    Springer
    Astrophysics and space science 26 (1974), S. 403-430 
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    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The spatial dependence of the pitch-angle and associated spatial diffusion coefficients for cosmic ray particles in interplanetary space is calculated in the WKB approximation. The model considers only Alfven waves of solar origin to be responsible for scattering of moderate energy particles. After developing the general theory results are presented for the asymptotic case corresponding to radial distancesr greater than about 1 to 2 AU. The radial diffusion coefficientи r increases with energyE likeи r ∼E υ, wherev≈2/3. The radial mean free path turns out to increase proportional tor 3 at medium and low heliographic latitudes. This behaviour is consistent with a very small radial cosmic ray gradient and the existence of a ‘free boundary’ for particle diffusion. At equal radial distances the high latitude mean free path is not only much smaller than the one calculated at the lower latitudes but in addition increases only weakly with distance. Some conceivable dynamical implications for the outer solar system are indicated.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00645623
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  • 7
    Electronic Resource
    Electronic Resource
    Cosmic-ray acceleration and transport, and diffuse galactic γ-ray emission (1983)
    Springer
    Space science reviews 36 (1983), S. 3-25 
    Details
    ISSN: 1572-9672
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Cosmic-ray acceleration and transport is considered from the point of view of application to diffuse galactic γ-ray sources. As an introduction we review several source models, in particular supernovae exploding inside or near large interstellar clouds. The complex problem of cosmic ray transport in random electromagnetic fields is reduced to three cases which should be sufficient for practical purposes. As far as diffusive acceleration is concerned, apart from reviewing the basic physical principles, we point out the relation between shock acceleration and 2nd order Fermi acceleration, and the relative importance of the two processes around interstellar shock waves. For γ-ray source models the interaction of cosmic rays with dense clouds assumes great importance. Past discussions had been confined to static interactions of clouds with the ambient medium in the sense that no large scale mass motions in the ambient interstellar medium were considered. The well-known result then is that down to some tens of MeV or less, cosmic-ray nucleons should freely penetrate molecular clouds of typical masses and sizes. The self-exclusion of very low energy nucleons however may affect electron transport with consequences for the Bremsstrahlung γ-luminosity of such clouds. In this paper we consider also the dynamical interaction of dense clouds with a surrounding hot interstellar medium. Through cloud evaporation and accretion there exist mass flows in the cloud surroundings. We argue that in the case of (small) cloud evaporation the galactic cosmic rays will be essentially excluded from the clouds. The dynamic effects of cosmic rays on the flow should be minor in this case. For the opposite case of gas accretion onto (large) clouds, cosmic-ray effects on the flow will in general be large, limiting the cosmic-ray compression inside the cloud to dynamic pressure equilibrium. This should have a number of interesting and new consequences for γ-ray astronomy. A first, qualitative discussion is given in the last section.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00171897
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  • 8
    Electronic Resource
    Electronic Resource
    The propagation of Alfvén waves and their directional anisotropy in the solar wind (1973)
    Springer
    Astrophysics and space science 20 (1973), S. 267-285 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The propagation of solar Alfvén waves in interplanetary space is studied in the approximation of geometrical optics. Ray paths and the change of wave vectors and amplitudes along the rays are determined assuming an Archimedean-spiral interplanetary magnetic field. In particular, the Alfvénic fluctuations in the 2 directions perpendicular to the magnetic field direction are calculated under the assumption that the Alfvén waves are produced at the Sun and emitted with an isotropic directional distribution from a reference level close to the Sun. It turns out that due to the combined effect of spherical expansion of the solar wind flow and the spiralling of the interplanetary field the magnetic fluctuations in the direction perpendicular both to the unperturbed field and the radial direction have much more power than in the other directions (directional anisotropy). Our results are compared with spacecraft observations made by Belcher and Davis (1971), that show an anisotropy of a similar character. It is argued that under average conditions the physical process leading to an anisotropy is not selective coupling of Alfvén waves into compressional waves, as suggested by Belcher and Davis, but rather the above mentioned dissipationfree effect of geometrical optics. Finally, arguments are presented to explain the discrepancy between the calculated high anisotropy and the measured low anisotropy in terms of finite amplitude effects and wavescattering.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00642204
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  • 9
    Electronic Resource
    Electronic Resource
    Microstructure of the solar wind (1975)
    Springer
    Space science reviews 17 (1975), S. 255-276 
    Details
    ISSN: 1572-9672
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract In this review microstructure is understood to summarize the dynamical properties of the solar wind that enter the fluid equations, usually employed to describe the overall flow, only in one or the other averaged form. Thus, first a description of the kinetic picture of the solar wind is given; it mainly involves the structure of the particle distributions in velocity space and associated instabilities. Waves and discontinuities are discussed next. Two selected examples are mentioned where the effects of waves and discontinuities play a role. Specific physical properties of the interplanetary magnetic irregularity spectrum and its relevance for cosmic ray propagation are discussed at the end.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00718576
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  • 10
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    Maximum energy of cosmic-ray particles accelerated by supernova remnant shocks in stellar wind cavities (1988)
    Institute of Physics
    Details
    Publication Date: 1988-10-01
    Print ISSN: 0004-637X
    Electronic ISSN: 1538-4357
    Topics: Physics
    Published by Institute of Physics
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