Oblique MHD cosmic-ray modified shocks
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Oblique MHD cosmic-ray modified shocks two-fluid numerical simulations by Adam Frank

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Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, [Springfield, Va .
Written in English

Subjects:

  • Cosmic rays.,
  • Shock waves.

Book details:

Edition Notes

StatementAdam Frank, T.W. Jones, and Dongsu Ryu.
SeriesNASA contractor report -- NASA CR-192930.
ContributionsJones, T. W., Ryu, Dongsu., United States. National Aeronautics and Space Administration.
The Physical Object
FormatMicroform
Pagination1 v.
ID Numbers
Open LibraryOL15374368M

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This is the issue of "cosmic-ray-mediated" shocks discussed by Terasawa et al. () for two additional interplanetary shocks. This is a fascinating process that can be observed, in situ, at some. S.V. Chalov, Instability of the structure of strong oblique MHD cosmic-ray shocks. Astrophys. Space Sci. , – (b) ADS CrossRef zbMATH Google ScholarCited by: 2. @article{osti_, title = {THREE-DIMENSIONAL SIMULATIONS OF MAGNETOHYDRODYNAMIC TURBULENCE BEHIND RELATIVISTIC SHOCK WAVES AND THEIR IMPLICATIONS FOR GAMMA-RAY BURSTS}, author = {Inoue, Tsuyoshi and Asano, Katsuaki and Ioka, Kunihito}, abstractNote = {Relativistic astrophysical phenomena such as gamma-ray bursts (GRBs) . A. Abramovici et al. Graviational wave astrophysics. In E. W. Kolb and R. D. Peccei, editors, Particle and Nuclear Astrophysics and Cosmology in the Next Millennium, Proc. Snowmass Summer School, pages –World Scientific, Google ScholarCited by:

Chapter 9 - Global and modified shocks pp Get access. The structure of cosmic ray shocks. Astron. Astrophys., , The injection and acceleration of particles in oblique shocks–A unified Monte Carlo description. Astrophys. J., , Cited by: 7. Cosmic Ray Interactions, Propagation, and Acceleration in Space Plasmas (Astrophysics and Space Science Library) The book ends with a list providing more than 1, full references, a discussion on future developments and unsolved problems, as well as . The spectral index can be modified over time by various processes (e.g., wave‐particle interaction) that can move the plasma toward or away from the thermal equilibrium. This population is predominantly controlled by the upstream solar wind conditions, including the Cited by: We have applied a modified total variation diminishing (TVD) method within the framework of a finite difference method for solving a transport equation for cosmic rays in an irregular magnetic field. We employ Roe's superbee scheme to control the numerical Cited by:

A typical scenario for such a model is high-energy cosmic-ray feedback on the background plasma upstream of nonrelativistic SNR shocks. The model treats cosmic rays in a kinetic PIC way, while the ions and electrons of the thermal plasma are described through MHD equations [77], [78], [79].Author: Martin Pohl, Masahiro Hoshino, Jacek Niemiec. ASTM Astrophysical Plasmas Lecture notes (QMUL), astronomy, astrophysics, cosmology, general relativity, quantum mechanics, physics, university degree, lecture. () The challenges of modelling microphysics: ambipolar diffusion, chemistry, and cosmic rays in MHD shocks. Monthly Notices of the Royal Astronomical Society , () A New HLLD Riemann Solver with Boris Correction for Reducing Alfvén by: These shocks, depending on the direction of the upstream magnetic field, are distinguished as quasi-perpendicular and quasi-parallel shocks which exhibit different behaviours, reflecting particles back upstream and generating high electromagnetic wave intensities. Particle acceleration and turbulence at such shocks become possible and important.