Solar plasma flow past the moon
Solar wind interaction with moon derived for model and compared with satellite data
Behannon, K. W.↗
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Hydromagnetic aspects of solar wind flow past the moon
Solar wind interaction with moon, constructing mathematical model based on MHD equations and Explorer 35 data
Marsh, M. C.↗
Solar-wind flow past objects in the solar system
Solar wind interaction with earth, moon, Venus and Mars, reviewing literature on continuum fluid model, spacecraft observations, plasma characteristics, etc
Alksne, A. Y.↗
Solar-wind flow past the planets Earth, Mars, and Venus
Numerical analysis of solar wind interactions with nonmagnetic planets based on equations of magnetohydrodynamics for perfect gas
Rizzi, A. W.↗
Magnetic observations of the lunar cavity
Lunar diamagnetic cavity signatures from Ames magnetometer experiment on Explorer 35 orbiter, indicating solar wind interaction
Colburn, D. S.↗
Review of magnetic field observations
Recent observations of magnetic fields in the magnetosphere are reviewed, and critical experiments and data are identified for theoretical analysis and interpretation. Quantitative studies of the solar wind interaction with the earth's magnetic field, regional measurements near the earth's equator at R = 2-8 R sub E, the polar cusp region of the geomagnetosphere, and structural models of the neutral sheet region in the geomagnetic tail are considered.
Ness, N. F.↗
Stability of the Venus ionopause
The ionopause of the Venus ionosphere, as indicated by Mariner 5 electron density data, and which occurs at 500km on the day side, and 2500km on the night side is discussed in terms of the solar wind interaction with the ionosphere. It is concluded that for a source of stabilization by heating to be effective, a small horizontal magnetic field is required to reduce the downward heat conduction of charged particles, and it has been shown that such a magnetic field is present.
Herman, J.↗
Two early missions to the comets.
Early missions to the comets Grigg-Skjellerup in 1977 and Encke in 1980 are suggested as precursors to more ambitious missions to Encke rendezvous in 1984 and Halley intercept in 1986. The spacecraft structures, power systems, telemetry, configurations, and launch vehicles considered appropriate for these two missions are actual equipments ready for applications. The mission objectives would be exploration of the nature of the solar wind interaction with comets, the composition of the gaseous cometary atmosphere, and possibly the details of the trailing portion of a comet (ion and dust tails).
Farquhar, R. W.↗
Missions to comets
Missions to comets are outlined that form the basis for a new program to send a space probe to a comet. Simple flythroughs of the comet head will provide information about the composition of the ionized and neutral particles that make up the cometary atmosphere and on effects of solar-wind interaction with the comet. Projected are missions to the comets Grigg-Skjellerup, Encke, and Halley.
Farquhar, R. W.↗
Study of carbon compounds in Apollo 12 and 14 lunar samples.
The results of gas-chromatography and high-resolution mass spectroscopy studies of gases released on deuterium fluoride dissolution of Apollo 12 and 14 lunar samples are reported. The results confirm previous observations that CH4 and C2H6 are released as well as CD4, C2D4, C2D6, and higher deuterated hydrocarbons. The yields correlate with the total carbon content of the samples, and the CH4 and C2H6 released may be regarded as indigenous, while the deuterated products result from hydrolysis of carbide material. The results provide the first experimental confirmation of the hypothesis that the CH4 derives from solar wind interactions.
Holland, P. T.↗
Comet exploration - Scientific objectives and mission strategy for a rendezvous with comet Encke.
A rendezvous mission which includes an extended stay of 80 days or longer in the vicinity of the comet is considered. Such a mission with exploration maneuvers through the coma and tail and circumnavigation of the nucleus is made feasible by the use of solar-electric propulsion. The physical characteristics of comet Encke are examined, giving attention to the icy conglomerate model of the nucleus, solar wind interaction, and chemical composition. Scientific objections are discussed together with mission profile options.
Meissinger, H. F.↗
Apollo particles and fields subsatellite magnetometer experiment
The results of the Apollo 15 subsatellite magnetometer experiment are reported. The magnetometer is described including the operation, and specifications. Orbit plots presented are altitude versus time, selenographic longitude versus latitude, and the ecliptic projection of the earth-moon system. The lunar magnetic field, solar wind interaction with the moon, the transfer function of the moon, and the plasma sheet interaction with the moon are discussed.
Coleman, P. J., Jr.↗
Global electromagnetic induction in the moon and planets
Experiments and analyses concerning electromagnetic induction in the moon and other extraterrestrial bodies are summarized. The theory of classical electromagnetic induction in a sphere is first considered, and this treatment is extended to the case of the moon, where poloidal eddy-current response has been found experimentally to dominate other induction modes. Analysis of lunar poloidal induction yields lunar internal electrical conductivity and temperature profiles. Two poloidal-induction analytical techniques are discussed: a transient-response method applied to time-series magnetometer data, and a harmonic-analysis method applied to data numerically Fourier-transformed to the frequency domain, with emphasis on the former technique. Attention is given to complicating effects of the solar wind interaction with both induced poloidal fields and remanent steady fields. The static magnetization field induction mode is described, from which are calculated bulk magnetic permeability profiles. Magnetic field measurements obtained from the moon and from fly-bys of Venus and Mars are studied to determine the feasibility of extending theoretical and experimental induction techniques to other bodies in the solar system.
Dyal, P.↗
Observations at Venus encounter by the plasma science experiment on Mariner 10
Preliminary results from the rearward-looking electrostatic analyzer of the plasma science experiment during the Mariner 10 encounter with Venus are described. They show that the solar-wind interaction with the planet probably involves a bow shock rather than an extended exosphere, but that this is not a thin boundary at the point where it was crossed by Mariner 10. An observed reduction in the flux of electrons with energies greater than 100 electron volts is interpreted as evidence for some direct interaction with the exosphere. Unusual intermittent features observed downstream of the planet indicate the presence of a comet-like tail hundreds of scale lengths in length.
Bridge, H. S.↗
Mariner 10 Mercury encounter
Mariner 10's closest approach to Mercury on Mar. 29, 1974 occurred on the dark side of the planet at a range of approximately 700 kilometers. The spacecraft trajectory passed through the shadows of both the sun and earth. Experiments conducted included magnetic fields, plasma and charged particle studies of the solar wind interaction region, television photography, extreme ultraviolet spectroscopy of the atmosphere, the detection of infrared thermal radiation from the surface, and a dual-frequency radio occultation in search of an ionosphere.
Dunne, J. A.↗
Effect of the frozen-in magnetic field on the formation of Venus, plasma shell boundary: Experimental confirmation
A laboratory simulation of solar wind interaction with plasma shells of nonmagnetic planets is reported. It is shown that the momentum transfer from the plasma flow to the shell occurs due to the presence of a frozen-in magnetic field. Without a magnetic field frozen-in, the ionosphere has no sharp boundary and a shock wave does not form in the flow.
Andrijanov, J. V.↗
Ongoing data reduction, theoretical studies
A nonspecific review of theory, correlative date analysis and supporting research and technology is presented. Title pages in some of the following areas are included: (1) magnetosphere boundary observations; (2) venus ionosphere and solar wind interaction; (3) ISEE-C plasma wave investigation, and (4) solar system plasmas.
Scarf, F. L.↗
Jupiter's magnetic tail: Voyager 1
Magnetic field observations by the Voyager 1 spacecraft during the outbound traversal of the Jovian magnetosphere in March 1979 suggest the detection of an extended magnetic tail, which has been formed by the solar wind interaction with the planetary field. The apparent diameter of the tail is 300-400 times the radius of Jupiter but its length is not measured. When combined with the GSFC O4 model of the planetary field, this magnetosphere topology leads to polar cap auroral zones approximately 20 deg in diameter, considerably smaller than earth's. The northern zone is found to be highly eccentric, encircling neither the rotational pole nor the magnetic pole of Jupiter, and limited to System III (1965) longitudes approximately 133 deg to 190 deg and latitudes approximately 62 deg to 82 deg.
Ness, N. F.↗