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Wednesday, August 5, 2020 | History

3 edition of **Alfve n wave transport effects in the time evolution of a parallel cosmic-ray modified shocks** found in the catalog.

Alfve n wave transport effects in the time evolution of a parallel cosmic-ray modified shocks

- 218 Want to read
- 40 Currently reading

Published
**1993**
by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, [Springfield, Va
.

Written in English

- Cosmic rays.,
- Shock waves.

**Edition Notes**

Statement | T.W. Jones. |

Series | [NASA contractor report] -- NASA CR-192932., NASA contractor report -- NASA CR-192932. |

Contributions | United States. National Aeronautics and Space Administration. |

The Physical Object | |
---|---|

Format | Microform |

Pagination | 1 v. |

ID Numbers | |

Open Library | OL14692916M |

Nonlinear evolution of Alfven waves. Nonlinear evolution of relativistic ring instability. Soliton acceleration: relativistic effects. Cross-field transport of cosmic rays. On nonstationarity of super-critical perpendicular shocks. Multiscale reconnection in the magnetotail. Mulit-scale reconnection in the earth's. Abstract. We present calculations of expected continuum emissions from Sedov–Taylor phase Type Ia supernova remnants (SNRs), using the energy spectra of cosmic.

Cosmic Ray Interactions, Propagation, and Acceleration in Space Plasmas (Astrophysics and Space Science Library) Chapter 3 is devoted to CR non-linear effects in space plasmas caused by CR pressure and CR kinetic stream instabilities with the generation of Alfv?n turbulence. The book ends with a list providing more than 1, full. Effects of electron heat conduction were identified as an important factor in the wave evolution. This area is ripe for a meaningful comparison with astrophysical observations. The Interaction of dense clumps with hypersonic flows is also a well-established area with connections to a variety of astrophysical phenomena.

Long time evolution of a nonlinear Alfven wave in a strongly relativistic electron-positron plasma and associated partcle acceleration. Numerical simulation on an electron-positron shock wave including a cosmic ray component. Responses of a cylindrical plasma to external electromagnetic field: analytical theory and numerical. Cosmic Ray Transport Equation for DSA Acceleration Efficiency (AE) depends on (1) Alfvenic drift: intensities of forward and backward waves Alfven wave (self-generated) X A 5 k -Evolution of weak shocks is almost test-particle.-No modification to the shock flow.-p_inj determines P_cr g (p) f (p) p4.

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Abstract. This paper presents a numerical study of the time evolution of plane, cosmic-ray modified shocks with magnetic field parallel to the shock normal, based on the diffusive shock acceleration formalism and including the effects from the finite propagation speed and energy of Alfven waves responsible for controlling the transport of the cosmic by: Get this from a library.

Alfvén wave transport effects in the time evolution of a parallel cosmic-ray modified shocks. [T W Jones; United States. National Aeronautics and. Abstract. This paper presents a numerical study of the time evolution of plane, cosmic-ray modified shocks with magnetic field parallel to the shock normal, based on the diffusive shock acceleration formalism and including the effects from the finite propagation speed and energy of Alfven waves responsible for controlling the transport of the cosmic : T.

Jones. It is also clear, however, that the impact of Alfven transport effects, which tend to slow shock evolution and reduce the time asymptotic cosmic-ray pressure in.

Time evolution of plane, cosmic-ray modified shocks has been simulated numerically for the case with parallel magnetic fields. Computations were done in a "three-fluid" dynamical model incorporating cosmic-ray and Alfvén-wave energy transport by: 5. Alfv4n Wave Transport Effects in the Time Evolution of Parallel Coslnic-Ray Modified Shocks T.

Jones Department of Astronomy, University of Minnesota, Minneapolis, MN To be published in the Astrophysical Journal Aug (NASA-CR) ALFVEN WAVE TRANSPORT EFFECTS IN THE TIME EVOLUTION OF PARALLEL COSMIC-RAY. Alfven wave transport effects in the time evolution of parallel cosmic-raymodified shocks.

Ap.J., –, The ponderomotive force due to cosmic ray generated Alfven waves. Time evolution of plane, cosmic-ray modified shocks has been simulated numerically for the case with parallel magnetic fields. Computations were done in a 'three-fluid' dynamical model incorporating cosmic-ray and Alfven-wave energy transport equations.

Nonlinear feedback from the cosmic rays and Alfven waves is included in the equation of motion for the underlying. SAO/NASA Astrophysics Data System (ADS) Title: Alfven wave transport effects in the time evolution of parallel cosmic-ray-modified shocks Authors: Jones, T.

Using an improved version of the previously introduced Cosmic Ray Acceleration SHock (CRASH) code, we have calculated the time evolution of cosmic-ray (CR) modified quasi-parallel plane shocks for Bohm-like diffusion, including self-consistent models of Alfvén wave drift and dissipation, along with “thermal leakage injection” of CRs.

teraction effects. The linearized wave evolution equations were used in Webb et al. (a,b,c,) to study the effect of wave mixing on the cosmic ray squeezing instability in cosmic-ray-modi ed shocks and ows.

Alfvenic models of cosmic-ray-modi ed shocks in which the Alfv en waves that. We use kinetic simulations of diffusive shock acceleration (DSA) to study the time-dependent evolution of plane, quasi-parallel, cosmic-ray (CR) modified shocks. Thermal leakage injection of low-energy CRs and finite Alfvén wave.

It is now well established that cosmic rays (CRs) are accelerated at collisionless shocks through diffusive shock acceleration.

However, some key physical processes, such as thermal leakage injection, self-excitation and dissipation of waves, and resonant scatterings of particles by those waves are nonlinear and not fully understood yet. Hence it is not possible to. Dispersion relations for the case of a magnetized plasma are determined taking into account the Hall current and a constant resistivity, {eta}, in Ohm's law.

It is found that the Hall effect is relevant only for parallel (to the equilibrium magnetic field) wave numbers in the case of uniform plasmas, giving place to a dispersive behavior. In gradual solar energetic particle (SEP) events, protons and heavy ions are often accelerated to > MeV/nucleon at a CME-driven shock.

In this work, we study particle acceleration at an oblique shock by extending our earlier particle acceleration and transport in heliosphere (PATH) code to include shocks with arbitrary θ BN, where θ BN is the angle.

Figure 2 shows the time evolution of the plasma density, that of the electric field E x and that of the magnetic field components B y and B z. The B x component cannot change since ∇ B = 0. The plasma density close to x = 0 increases to 2 after the simulation begins, due to the superposition of the inflowing and reflected plasma.

We solve the transport equation using a backward stochastic differential equation method where adiabatic cooling, focusing, pitch angle scattering, and cross‐field diffusion effects are all included. Time intensity profiles and instantaneous particle spectra as well as particle pitch angle distributions are shown for two example CME shocks.

This is an excellent time to do research on cosmic rays. Recent progress in radio, γ-ray, and particle detection capabilities together with improved understanding of magnetic turbulence, energetic particle transport, reconnection, and collisionless shocks, and advances in computation are making it possible to develop and test theoretical ideas in unprecedented.

Bieber JW, Wanner W, Matthaeus WH. Dominant two-dimensional solar wind turbulence with implications for cosmic ray transport. Geophys. Res. Bieber JW, Matthaeus WH. Perpendicular Diffusion and Drift at Intermediate Cosmic-Ray Energies. ApJ. Black JH, van Dishoeck EF.

@article{osti_, title = {GLOBAL SIMULATIONS OF GALACTIC WINDS INCLUDING COSMIC-RAY STREAMING}, author = {Ruszkowski, Mateusz and Yang, H.-Y. Karen and Zweibel, Ellen}, abstractNote = {Galactic outflows play an important role in galactic evolution.

Despite their importance, a detailed understanding of the physical mechanisms responsible for. In particular, if τ s is the time for spectral energy transfer due to wave-cascading and τ d is the damping time of waves on the relativistic particles, one has two relevant asymptotic cases.

For τ s «τ d, the spectrum of the waves is driven by the injection of Alfvén waves and the process of wave-cascading. Although the evolution of the shock in our time-dependent run into a CR-dominated state (Section ) is physical within the framework of the two-fluid theory (Section 2), the question of whether it is a realistic description of the subsequent evolution of the Balmer-dominated shock at knot g must be approached with care.

Our plane-parallel.Book Description: Until the advent of space physics, astrophysical plasmas could be studied only using ground-based observations. Although observational methods have advanced over recent decades, the merging of heliospheric physics with astrophysics is far from complete due to the vastly different techniques employed by astronomers and space physicists.