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Plasma conductivity for Comet Halley ionosphere
Observational as well as semitheoretical magnetic field profiles have been used to derive self-consistently the plasma conductivity profiles for the ionosphere of Comet Halley. The characteristic diffusion length for the field, according to the present model, is about 28 km; this is in very good agreement with the Giotto spacecraft observations. It is shown that ideal MHD as well as constant conductivity models are not appropriate for the study of dynamical structure of the Halley's ionosphere.
Plasma conductivity gage
Gage permits determination of stagnation conductivity from measurement of shunt impedance presented by the plasma between the inner and outer conductors of a segment of coaxial transmission line. Response of gage permits its use in shock-tube work and research on explosive propagation.
Experimental measurement of the plasma conductivity of Z93 and Z93P thermal control paint
Two samples each of Z93 and Z93P thermal control paint were exposed to a simulated space environment in a plasma chamber. The samples were biased through a series of voltages ranging from -200 volts to +300 volts and electron and ion currents measured. By comparing the currents to those of pure metal samples of the same size and shape, the conductivity of the samples was calculated. Measured conductivity was dependent on the bias potential in all cases. For Z93P, conductivity was approximately constant over much of the bias range and we find a value of 0.5 micro-mhos per square meter for both electron and ion current. For Z93, the dependence on bias was much more pronounced but conductivity can be said to be approximately one order of magnitude larger. In addition to presenting these results, this report documents all of the experimental data as well as the statistical analyses performed.
Effective Drag in Rotating, Poorly Conducting Plasma Turbulence
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A.c. conductivity of a plasma.
Conductivity of fully ionized spatially homogeneous plasma under uniform periodically alternating electric field
A conductivity probe for tenuous plasmas.
Conductivity probe design for tenuous plasmas and ionized gases, discussing experimental confirmation of theoretical behavior
A conductivity probe for tenuous plasmas.
Conductivity probe design for tenuous plasmas and ionized gases, discussing experimental confirmation of theoretical behavior
Kinetic equation for a plasma and its application to high frequency conductivity
Plasma kinetic equation applied to high frequency conductivity
A new determination of the thermal conductivity of nitrogen plasma.
Thermal conductivity of nitrogen plasma in cascade arc, solving Elenbaas-Heller equation
Thermal conductivities of plasmas in general force fields.
Plasma thermoconductivity in general force fields, showing validity of Meador-Staton results in case of ambipolar diffusion and nonuniform total pressure
High-frequency conductivity of a plasma in quasi-equilibrium. III - Study of a two- temperature plasma.
HF conductivity of quasi-equilibrium isotropic fully ionized two-temperature plasma
Comments on ''high-frequency conductivity of a fully ionized plasma.''
Error concerning existence of nonuniformity in article on plasma conductivity by Oberman, Ron and Dawson
Effect of resonant charge exchange on heat conduction in plasmas.
Cross section estimates for symmetric resonant charge exchange between ions differing by one electronic charge, noting effect on heat conduction in plasmas
Electric conductivity of plasma in solar wind
One of the most important parameters in MHD description of the solar wind is the electric conductivity of plasma. There exist now two quite different approaches to the evaluation of this parameter. In the first one a value of conductivity taken from the most elaborated current theory of plasma should be used in calculations. The second one deals with the empirical, phenomenological value of conductivity. E.g.: configuration of interplanetary magnetic field, stretched by the expanding corona, depends on the magnitude of electrical conductivity of plasma in the solar wind. Knowing the main empirical features of the field configuration, one may estimate the apparent phenomenological value of resistance. The estimations show that the electrical conductivity should be approximately 10(exp 13) times smaller than that calculated by Spitzer. It must be noted that the empirical value should be treated with caution. Due to the method of its obtaining it may be used only for 'large-scale' description of slow processes like coronal expansion. It cannot be valid for 'quick' processes, changing the state of plasma, like collisions with obstacles, e.g., planets and vehicles. The second approach is well known in large-scale planetary hydrodynamics, stemming from the ideas of phenomenological thermodynamics. It could formulate real problems which should be solved by modern plasma physics, oriented to be adequate for complicated processes in space.
Third-order contributions to electrical conduction in plasmas
Solution to modified Chapman-Enskog kinetic equation for calculating electrical conductivity of nonequilibrium plasma
Conditions for double layers in the Earth's magnetosphere and perhaps in other astrophysical objects
Double layers form along auroral field lines in the Earth's magnetosphere. They form in order to maintain current continuity in the ionosphere in the presence of a magnetospheric electric field E with nabla x E is not equal to 0. Features which govern the formation of the double layers are: (1) the divergence of E, (2) the conductivity of the ionosphere, and (3) the current-voltage characteristics of auroral magnetic field lines. Astrophysical situations where nabla x E is not equal to 0 is applied to a conducting plasma similar to the Earth's ionosphere are potential candidates for the formation of double layers. The region with nabla x E is not equal to 0 can be generated within, or along field lines connected to, the conducting plasma. In addition to nabla x E, shear neutral flow in the conducting plasma can also form double layers.
Plasma measurements conducted in the vincinity of Venus on the spacecraft VENERA-4
Plasma flux measurements in vicinity of Venus by charged particle traps on Venera-4 spacecraft