Wave‐induced chaotic radial transport of energetic electrons in a laboratory terrella experiment

1995 ◽  
Vol 2 (11) ◽  
pp. 4185-4194 ◽  
Author(s):  
H. P. Warren ◽  
M. E. Mauel
Keyword(s):  
Radial Transport ◽  
Energetic Electrons ◽  
Wave Induced

On radio-frequency wave-induced radial transport and wave helicity

1993 ◽  
Vol 49 (1) ◽  
pp. 55-62 ◽  
Author(s):  
V. A. Petržílka
Keyword(s):  
Radio Frequency ◽  
Cyclotron Resonance ◽  
Ion Cyclotron Resonance ◽  
Wave Polarization ◽  
Radial Transport ◽  
Magnetostatic Field ◽  
Frequency Wave ◽  
Ion Cyclotron ◽  
Radio Frequency Wave ◽  
Wave Induced

Expressions for wave-induced radial transport are derived, allowing simple estimates to be obtained. The transport is enhanced owing to the presence of a poloidal magnetostatic field and in the vicinity of ion-cyclotron resonance. The direction of the wave-induced transport also depends on the wave polarization.

Observation of wave‐induced chaotic radial transport in a laboratory terrella experiment

1996 ◽  
Vol 3 (5) ◽  
pp. 2143-2148 ◽  
Author(s):  
H. P. Warren ◽  
M. E. Mauel ◽  
D. Brennan ◽  
S. Taromina
Keyword(s):  
Radial Transport ◽  
Wave Induced

A new outlook at Uranus' and Neptune's 10 keV--5 MeV energy electron distributions from data analyses and physics-based models

2021 ◽  
Author(s):  
Daniel Santos-Costa
Keyword(s):  
Data Analysis ◽  
Theoretical Modeling ◽  
Spatial Distributions ◽  
Radial Transport ◽  
Modeling Tools ◽  
Energetic Electrons ◽  
Comparison Results ◽  
Electron Distributions ◽  
Sweeping Effect

<p>We present our latest understanding of the processes that shape the spatial distributions of energetic electrons trapped in the magnetospheres of Uranus (L < 15) and Neptune (L < 25). To determine what controls the energy and spatial distributions throughout the different magnetospheres, we compute the time evolution of particle distributions with the help of a diffusion theory particle transport code that solves the governing 3-D Fokker-Planck equation. Different mechanisms of particle loss, source and transport are numerically examined. Our theoretical modeling is guided by the analysis of particle, field and wave data collected during Voyager 2’s flyby of Uranus in January 1986 and at Neptune in August 1989.</p> <p>Our preliminary data-model comparison results at Uranus show that adiabatic transport cannot explain the radial and angular features of warm to ultra-relativistic electron populations within the ~1-15 L region. Our simulation results also suggest that, with absence of loss mechanisms inside L = 15, energetic and radiation-belt electron populations would be higher by 1-3 orders of magnitude in intensity close to the planet (L ~ 1-8). Particularly, our results confirm that moon sweeping effect is a significant loss mechanism at Uranus. Nonetheless, other radial, energy and pitch-angle dependent mechanisms seem to be missing to explain the in-situ data. We will thus present our ongoing effort to examine the role of --for instance, Uranus’ rings system, atomic hydrogen corona and wave activity inward of L ~ 8-10 to improve our modeling of Uranus’ electron populations between L values of 1 and 15.</p> <p>Our first physics-based model of energetic electrons at Neptune will be presented, emphasizing first the role of radial transport and moon sweeping effect for the 1-25 L region before investigating new processes. Our models developed for Uranus and Neptune are based on the theoretical modeling of electron distributions at Saturn, which included the modeling of radial transport and interactions of electrons with Saturn's dust/neutral/plasma environments and waves, as well as particle sources from high-latitudes, interchange injections, and outer magnetospheric region. Comparisons between the distributions of electron populations at Gas and Ice Giant systems will be discussed.</p> <p>Data analysis, theoretical modeling, and numerical computations for Uranus and Neptune are carried out by adapting the Kronian modeling tools developed at Southwest Research Institute to the Ice Giants environment. Key data analysis, theoretical modeling, and numerical computational tasks for Saturn were carried out at Southwest Research Institute under NASA GSFC grant 80NSSC18K1100.</p>

2D effect during the propagation of schock wave induced by laser plasma : Application for laser adherence test (LASAT)

2005 ◽  
Author(s):  
Laurent Berthe ◽  
Cyril Bolis ◽  
Michel Boustie ◽  
Michel Arrigoni ◽  
Sophie Barradas ◽  
...  
Keyword(s):  
Laser Plasma ◽  
Adherence Test ◽  
Wave Induced
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