Numerical simulation of rotation-driven plasma transport in the Jovian magnetospherefinal technical report on NASA grant NAGW-4035, period of grant: April 1, 1994 to December 31, 1997
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National Aeronautics and Space Administration, National Technical Information Service, distributor , [Washington, DC, Springfield, Va
Numerical analysis., Plasmas (Physics), Centrifugal force., Magnetospheres., Models., Im
|Other titles||Numerical simulation of rotation driven plasma transport in the Jovian magnetosphere.|
|Statement||principal investigator, Richard A. Wolf.|
|Series||[NASA contractor report] -- NASA/CR-208175., NASA contractor report -- NASA CR-208175.|
|Contributions||United States. National Aeronautics and Space Administration.|
|The Physical Object|
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A Jupiter version of the Rice Convection Model (RCM-J) was developed with support of an earlier NASA SR&T grant. The conversion from Earth to Jupiter included adding currents driven by centrifugal force, reversing the planetary magnetic field, and rescaling various parameters.
A series of informative runs was carried out, all of them solving initial Author: Richard A. Wolf. NASAJCR._. _- Final Technical Report on NASA Grant NAGW "Numerical Simulation of Rotation-Driven Plasma Transport in the Jovian Magnetosphere".
Numerical Simulation of Rotation-Driven Plasma Transport In the Jovian Magnetosphere. By Richard A. Wolf. Abstract. A Jupiter version of the Rice Convection Model (RCM-J) was developed with support of an earlier NASA SR&T grant.
The conversion from Earth to Jupiter included adding currents driven by centrifugal force, reversing the planetary Author: Richard A. Wolf. "Numerical simulation of rotation-driven plasma transport in the Jovian magnetosphere": final technical report on NASA grant NAGW, period of.
The numerical simulations of a heavy flux tube motion in the equilibrium models of Jupiter's inner magnetosphere for this period yield two results: (1) the heavy flux tube is unstable in a model with only cold plasma included and (2) the heavy flux tube is stable in models with both cold and hot plasma by: In this chapter we present a review of plasma transport in the magnetospheres of the rapidly rotating outer planets Jupiter and Saturn with emphasis on the effects of magnetic reconnection.
Unlike the Earth’s magnetosphere where reconnection is the dominant transport mechanism, atmospherically driven corotation dominates at Jupiter and by: 2.
A centrifugally confined plasma utilizes centrifugal forces from supersonic plasma rotation to augment the conventional magnetic confinement of fusion plasmas. Appropriately used, plasma pressure can be contained along the magnetic field lines, allowing for “open” configurations, introducing flexibility in design.
The axisymmetric equilibrium of one such system, a single coil configuration, is investigated by: 4. Galileo evidence for rapid interchange transport in the Io torus Numerical simula-tion of plasma transport driven by the Io torus Numerical simulation of torus-driven transport in the Jovian.
1 Introduction. A rotation‐driven planetary magnetosphere is powered, at least in part, by rotational energy extracted from the planet by active plasma sources operating within the magnetosphere [e.g., Dessler, ; Eviatar and Siscoe, ].The most thoroughly observed examples are the magnetospheres of Jupiter and Saturn, thanks largely to the orbital missions Cited by: 2.
Numerical experiments are performed to study the possibility of long-lived vortex generation in rotating convection zones. The domain of computation is a rectangular box with fixed latitude.
The fully compressible fluid equations are solved using an explicit, strongly conservative finite difference by: The most striking feature of the Jovian plasma-wave observations is the very close similarity to the plasma-wave phenomena observed in the earth's magnetosphere.
In a description of the plasma-wave results obtained with the aid of Voyager, the observed phenomena are discussed in several broad categories. Ioaniddis, N. Brice, Plasma densities in the Jovian magnetosphere: plasma slingshot or Maxwell demon.
Ica – (). doi: /(71) ADS Cited by: The departure of the Jovian magnetosphere from rigid corotation is adequately explained by outward plasma transport at distances L> or approx. = It is a magnetosphere whose physics is dominated by internal sources of plasma and energy.
This book consists of twelve carefully interwoven articles written by leading space scientists who summarize our state of knowledge of the physics of the magnetosphere Format: Paperback. Physics of the Jovian Magnetosphere by A. Dessler,available at Book Depository with free delivery worldwide.3/5(1).
S.J. Bolton et al. Fig. 1 (A) The magnetosphere of Jupiter extends 63–92 Jovian radii in the direction towards the Sun, with a tail that stretches beyond the orbit of Saturn >4 AU, and occupies a volume over a thousand times that of the Sun. (B) Intense auroral emissions are signatures of the coupling between the planet and the magnetospheric.
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An example map, Fig. 1 shows the normalized optical free–free emissivity in logarithmic scale. This map was created from simulation data taken at the snapshot time of wire-crossing times. At this time, the wind coming into the grid from the left side had deflected around the wire, and in the course of its navigation around the obstacle components of the magnetosphere Cited by: 3.
Advances in Dusty Plasmas. Proceedings of the International Conference on Physics of Dusty Plasmas. Numerical Simulation of Phase Transitions in Dense Dusty Plasmas.
Dust Crystals. Dust in the Jovian Magnetosphere: From the Smallest Moons to the Heaviest Plasma Species. radial distance of RJ (Jovian radii, 71,km) from Jupiter, and has a radius of km (1 RE). The interaction of Europa with the magnetized plasma of the Jovian plasma sheet gives rise to a so-called Alfv´en wing, which has been extensively studied in the case of Io (e.g., Neubauer, ; Southwood et al., ; Herbert, ; Lipatov Cited by: 9.
Description Numerical simulation of rotation-driven plasma transport in the Jovian magnetosphere PDF
rotating Jupiter magnetosphere with respect to the ﬂute per-turbations. Model radial distribution of the magnetic ﬁeld and experimental data on the plasma angular velocity in the middle Jovian magnetosphere are used.
A dispersion relation of the plasma perturbations in the case of a perfectly conduct-ing ionosphere is obtained. Nonlinear mechanisms of lower‐band and upper‐band VLF chorus emissions in the magnetosphere. Yoshiharu Omura.
Research Institute for Sustainable Humanosphere, Kyoto University, Kyoto, Japan Communications in Nonlinear Science and Numerical Simulation, / Pitch angle diffusion by whistler mode waves in the jovian.
A series of plasma voids ("dropouts") was observed by the Plasma Science (PLS) experiment in Jupiter's magnetosphere during the Voyager 2 encounter with that planet. A reexamination of Voyager 2 data has led us to conclude that the dropout phenomenon cannot be a manifestation of a plasma wake produced by Ganymede.
plasma sources in the close-in equatorial magnetosphere parallels conditions at Jupiter. This suggests that we need to study both Jupiter and Earth when thinking about what to anticipate from Cassinis exploration of Saturns magnetosphere.
This paper addresses issues relevant to plasma transport and acceleration in all three magnetospheres. Transport and entry of plasma clouds/jets across transverse magnetic discontinuities: Simulation setup The numerical simulations are performed in a three-dimensional geometry that allows the simultaneous investigation of the plasma.
The dynamic plasma flow of the Jovian magnetosphere shapes and distorts the draped field around the icy moons. In a km Ganymede orbit, the expected induction signal is 10’s of nT. The field perturbations from the plasma interactions are expected to be of the same order or more.
Measurements of the plasma. Dust Dynamics in Electrostatic Sheath of a Dusty Plasma; Self-Similar Expansion of Dust Grains in a Plasma; IV. Dusty Plasmas in the Atmosphere and Space. Dusty Plasmas in Environmental Research: Mitigation of Ozone Depletion Using Charged Liquid Droplets; Dust in the Jovian Magnetosphere: From the Smallest Moons to the Heaviest Plasma Species.
LFM simulation of the Jovian magnetosphere indicates the dawn-dusk asymmetry in Kelvin-Helmholtz waves, a Rayleigh-Taylor-like instability in the inner magnetosphere, magnetic plasmoids shed by the night side reconnection line, as well as the auroral signatures on the inset in the lower left corner.
NUMERICAL SIMULATION OF HEAT AND MASS TRANSPORT-DURING SPACE CRYSTAL GROWTH WITH MEPHISTO Minwu Yao Ohio Aerospace Institute, Brook Park, OH Raghu Raman University of Florida, Gainesville, FL Henry C.
Details Numerical simulation of rotation-driven plasma transport in the Jovian magnetosphere FB2
de Groh llI NASA Lewis Research Center, MS 10S-l, Cleveland, OH ABSTRACT The MEPHISTO space experiments are. 18 Belcher ' Low Energy Plasma in the Jovian Magnetosphere function, and Y Ij/•'j is proportional to the density N. This assumes that U n is less than 9i•, the average velocity of our highest channel.
The currents measured in the Jovian magnetosphere are due to many ionic species. Frequently, these species are hot enough so that.
In the present work, the Direct Simulation Monte Carlo (DSMC) method is used to simulate the interaction of Io's atmosphere with the Jovian plasma torus and the results are compared to observations. These comparisons help constrain the relative contributions of atmospheric support as well as highlight the most important physics in Io's atmosphere.
Listed below are references to journal and book articles that are related to our Dusty Plasma Experiment as well as the Dusty Plasma field. This database will be updated frequently.
Last updated: 3/ Return to Main Page.of the Jovian magnetosphere to a northward IMF turning. The summary is in section 6. 2. Simulation Model  Our simulation model of the solar wind interaction with Jupiter’s rapidly rotating magnetosphere has been described by Ogino et al.
. In this section we briefly review the simulation model and show how this calcula.His research focuses on comparative magnetospheric physics with an emphasis on the numerical simulation of space plasmas using hybrid (kinetic ion, fluid electron) and multi-fluid techniques.
Dr. Delamere has studied the solar wind interaction with the giant magnetospheres of Jupiter and Saturn, comets, Pluto and the plasma interaction at Io.
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