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M. Scholer 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1981,1(3):121-124
Numerical models of impulsive solar flare particle events usually assume the radial diffusion coefficient to be independent of energy per nucleon, T, although the observations indicate a T0.5 dependence (constant mean free path). The assumption of a constant diffusion coefficient results in a preservation of a power law injection spectrum at all radial distances throughout the event. We investigate the effect of an energy dependent diffusion coefficient on the spectrum of flux maxima at a fixed point in interplanetary space. This spectrum is harder than that of initial differential number densities close to the sun. Furthermore, the spectrum hardens with increasing radial distance which seems to be at variance with observations. 相似文献
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Shocks in collisionless plasmas require dissipation mechanisms which couple fields and particles at scales much less than the conventional collisional mean free path. For quasi-parallel geometries, where the upstream magnetic field makes a small angle to the shock normal direction, wave-particle coupling produces a broad transition zone with large amplitude, nonlinear magnetic pulsations playing an important role. At high Mach numbers, ion reflection and acceleration are dominant processes which control the structure and dissipation at the shock. Accelerated particles produce a precursor, or foreshock, characterized by low frequency magnetic waves which are convected by the plasma flow into the shock transition zone. The interplay between energetic particles, waves, ion reflection and acceleration leads to a complicated interdependent system. This review discusses the spacecraft observations which have motivated the current view of the high Mach number quasi-parallel shock, and the theories and simulation studies which have led to a better understanding of the microphysics on which the quasi-parallel shock depends. 相似文献
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THE CLUSTER ION SPECTROMETRY (CIS) EXPERIMENT 总被引:5,自引:0,他引:5
H. RÈME J. M. Bosqued J. A. Sauvaud A. Cros J. Dandouras C. Aoustin J. Bouyssou Th. Camus J. Cuvilo C. Martz J. L. MÉDALE H. Perrier D. Romefort J. Rouzaud C. D'Uston E. MÖBIUS K. Crocker M. Granoff L. M. Kistler M. Popecki D. Hovestadt B. Klecker G. Paschmann M. Scholer C. W. Carlson D. W. Curtis R. P. Lin J. P. Mcfadden V. Formisano E. Amata M. B. Bavassano-CATTANEO P. Baldetti G. Belluci R. Bruno G. Chionchio A. Di Lellis E. G. Shelley A. G. Ghielmetti W. Lennartsson A. Korth H. Rosenbauer R. Lundin S. Olsen G. K. Parks M. Mccarthy H. Balsiger 《Space Science Reviews》1997,79(1-2):303-350
The Cluster Ion Spectrometry (CIS) experiment is a comprehensive ionic plasma spectrometry package on-board the four Cluster spacecraft capable of obtaining full three-dimensional ion distributions with good time resolution (one spacecraft spin) with mass per charge composition determination. The requirements to cover the scientific objectives cannot be met with a single instrument. The CIS package therefore consists of two different instruments, a Hot Ion Analyser (HIA) and a time-of-flight ion COmposition and DIstribution Function analyser (CODIF), plus a sophisticated dual-processor-based instrument-control and Data-Processing System (DPS), which permits extensive on-board data-processing. Both analysers use symmetric optics resulting in continuous, uniform, and well-characterised phase space coverage. CODIF measures the distributions of the major ions (H+, He+, He++, and O+) with energies from ~0 to 40 keV/e with medium (22.5°) angular resolution and two different sensitivities. HIA does not offer mass resolution but, also having two different sensitivities, increases the dynamic range, and has an angular resolution capability (5.6° × 5.6°) adequate for ion-beam and solar-wind measurements. 相似文献
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Lembege B. Giacalone J. Scholer M. Hada T. Hoshino M. Krasnoselskikh V. Kucharek H. Savoini P. Terasawa T. 《Space Science Reviews》2004,110(3-4):161-226
The physics of collisionless shocks is a very broad topic, which has been well studied for many decades. However, there are a number of important issues which remain unresolved. Moreover, there have been new findings, which cast doubt on well-established ideas. The purpose of this review is to address a subset of unresolved problems in collisionless shock physics from a theoretical and/or numerical modeling point of view. The topics which are addressed are: the nonstationarity of the shock front, the heating and dynamics of electrons through the shock layer, particle diffusion in turbulent electric and magnetic fields, particle acceleration, and the interaction of pickup ions with collisionless shocks. 相似文献
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Manfred Scholer 《Space Science Reviews》1975,17(1):3-44
Whereas the entry mechanism of energetic solar particles into the open field line region of the magnetosphere is now a rather well understood process, transport processes of solar particles in the closed field line region are still unclear and under dispute. The main difficulty lies not only in the fact that different field models predict different behavior of the particles in the quasi-trapping region (e.g. cut-off latitude), but that dynamic changes of the magnetosphere as geomagnetic storms and substorms greatly influence the particle distribution. The present review tries to summarize the status of knowledge regarding solar proton behavior on closed magnetospheric field lines. Together with a presentation of recent measurements in the closed field line region relevant theoretical problems are discussed. They fall either under the study of single particle motion in different static magnetospheric configurations (due to different field models or due to real, e.g. ring current induced changes), or under the study of resonant interaction processes as pitch angle scattering and radial diffusion.Invited Lecture, Second Meeting of the European Geophysical Society, September 1974, Trieste, Italy. 相似文献
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An increasing number of high-resolution spacecraft observations provide access to details of energetic electron and ion velocity-space
distribution structures. Since resonant wave-particle interaction processes depend considerably on the distribution function
details, space plasma modeling is of particular interest for studies of a variety of plasma environments as planetary magnetospheres,
the interplanetary medium or solar flares. After summarizing the most popular particle acceleration processes we focus on
wave-powered energization mechanisms induced by Landau interaction and demonstrate from a time-evolutionary scenario that
power-law distributions, highly favored by observations in recent years, are generated resonantly by an Alfvén wave spectrum
and possibly saturate. This process is further stimulated in non-uniform magnetic field configurations where multiple wave
packets at different phase velocities provide the energy source for a continuous acceleration process. Moreover, in this conjunction
we demonstrate that in particular κ-distributions are a consequence of a generalized entropy concept, favored by nonextensive
statistics, which provides the missing link for power-law plasma models from fundamental physics. With regard to in situ space
observations examples are provided illuminating that for non-thermal plasma characteristics the particular structure of the
velocity-space distribution dominates as regulating mechanism for the wave-particle interaction process over effects related
to changes in space plasma parameters.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
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F Jamitzky M Scholer 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1997,19(12):1773-1776
Numerical simulations of magnetic reconnection with uniform resistivity show that the length of the current sheet increases for increasing magnetic Reynolds number. In order to prevent the current sheet from growing in general the resistivity is assumed to be localized. For uniform resistivity the reconnection proceeds much slower than for localized resistivity. In this paper analytical solutions of the hydromagnetic equation are presented for localized and uniform resistivity. It is shown that there exists an essential singularity in the behaviour of a solution of magnetic reconnection in the limit of large magnetic Reynolds number: For prescribed boundary conditions the solution for localized resistivity does not approach the solution for uniform resistivity in the limit of large magnetic Reynolds number. 相似文献