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  • 1
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    The dayside ionosphere of Venus (1971)
    In:  Other Sources
    Details
    Publication Date: 2011-08-16
    Description: Ionic and thermal structure model of daytime Venus ionosphere with solar wind heating based on Mariner 5 flyby mission
    Keywords: SPACE SCIENCES
    Type: ; ECTRON (
    Format: text
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  • 2
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    Model for rotating and nonuniform planetary exospheres. (1971)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: The model neutral exosphere with a uniformly rotating exobase is generalized by allowing variations in exobase density and temperature which characterize the thermosphere just below the base. The corresponding velocity distribution function, satisfying the collisionless Boltzmann equation, is constructed and used to form a general expression for the velocity moments. Resulting density profiles of rotating exospheres with nonuniform densities and temperatures on the exobase are compared with corresponding nonrotating exospheres. Density enhancements due to rotation are found to be greatest above regions of exobase density or temperature minima. Equatorial density enhancements of terrestrial hydrogen, resulting from rotation, are estimated to be 15%-17% at altitudes of 10-20 earth radii. Corresponding increases in terrestrial helium are 30%-50% on the equator at altitudes of 0.7 to 1 earth radii even when there is a polar density bulge in the barosphere.
    Keywords: SPACE SCIENCES
    Type: Physics of Fluids; 14; Dec. 197
    Format: text
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  • 3
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    Observations at Venus encounter by the plasma science experiment on Mariner 10 (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: 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.
    Keywords: SPACE SCIENCES
    Type: Science; 183; Mar. 29
    Format: text
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  • 4
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    Simple model for a rotating neutral planetary exosphere. (1969)
    In:  Other Sources
    Details
    Publication Date: 2011-08-12
    Description: Neutral exosphere model for nonrotating planet permitting barosphere uniform rotation at certain angular velocity, determining velocity distribution and density
    Keywords: SPACE SCIENCES
    Type: ; TROPHYSICAL JOURNAL
    Format: text
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  • 5
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    Topside ionosphere of Venus and its interaction with the solar wind (1970)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Solar wind and Venus topside ionosphere interaction, discussing charged particle density, temperature and pressure distribution
    Keywords: SPACE SCIENCES
    Type: ; TROPHYSICAL JOURNAL
    Format: text
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  • 6
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    Observations at Mercury encounter by the plasma science experiment on Mariner 10 (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: A fully developed bow shock and magnetosheath were observed near Mercury, providing unambiguous evidence for a strong interaction between Mercury and the solar wind. Inside the sheath there is a distinct region analogous to the magnetosphere or magnetotail of earth, populated by electrons with lower density and higher temperature than the electrons observed in the solar wind or magnetosheath. At the time of encounter, conditions were such that a perpendicular shock was observed on the inbound leg and a parallel shock was observed on the outbound leg of the trajectory, and energetic plasma electron events were detected upstream from the outbound shock crossing. The interaction is most likely not atmospheric, but the data clearly indicate that the obstacle to solar wind flow is magnetic, either intrinsic or induced.
    Keywords: SPACE SCIENCES
    Type: Science; 185; July 12
    Format: text
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  • 7
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    On the extent of the Martian ionosphere. (1973)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: The boundary of the Martian ionosphere just above the photochemical layer, where solar-wind induced convection becomes important, is estimated. The Martian ionosphere is expected to terminate at an altitude of approximately 300 km.
    Keywords: SPACE SCIENCES
    Type: Journal of Geophysical Research; 78; June 1
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  • 8
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    Venus ionosphere - An interpretation of Mariner 10 observations (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: The dayside ionosphere of Venus observed by Mariner 10 may be understood in terms of a dynamic interaction with the solar wind which results in a compressed topside above an 'F2 ledge' consisting of O(+) and a dynamically unaffected F1 layer corresponding to a neutral temperature of about 380 K and consisting of O2(+) and CO2(+). The top of the upper ledge appears to be an ionopause caused by solar wind scavenging of He(+), representing a solar-wind obstacle consistent with the bow shock observations.
    Keywords: SPACE SCIENCES
    Type: Geophysical Research Letters; 1; May 1974
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  • 9
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    The topside ionosphere of Venus and its interaction with the solar wind (1969)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Topside ionosphere of Venus and interaction with solar wind using Mariner 5 two frequency experiment
    Keywords: SPACE SCIENCES
    Type: NASA-TM-X-63717 , X-615-69-459
    Format: application/pdf
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  • 10
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    Preliminary report of results from the plasma science experiment on Mariner 10 (1974)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: Preliminary measurements of electron number density and temperature near Venus and Mercury and some results on flow speeds are presented. It is concluded that the interaction of the solar wind with Venus probably results in a bow shock characterized by H/r = 0.01 (ratio of the ionospheric scale height to the planetocentric distance of the nose of the ionopause); an extended exosphere appears unlikely. This direct interaction is indicated by the behavior of electrons with energies of 100-500 eV. Some unusual downstream effects suggest a comet-like tail several hundred scale lengths long. Near Mercury, a fully developed bow shock and magnetosheath were observed. Inside the magnetosheath there is a region analogous to the magnetosphere of the earth and populated by electrons of lower density and temperature than those found in the solar wind. The solar wind ram pressure corresponds to a stagnation pressure equivalent to a 170 gamma magnetic field. The strong solar wind interaction with Mercury is definitely magnetic, but not ionospheric or atmospheric. Spectra and particle flux varied widely while the spaceship was within the magnetosphere itself; temporal events like substorms may be responsible.
    Keywords: SPACE SCIENCES
    Type: Plenary Meeting; Jun 17, 1974 - Jul 01, 1974; Sao Paulo; Brazil
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