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  • LUNAR AND PLANETARY EXPLORATION  (46)
  • Solar Physics  (33)
  • 1995-1999  (35)
  • 1985-1989  (44)
  • 1
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    Evidence for Highly Inhomogeneous mm-Wave Sources During the Impulsive Flare of May 9, 1991 (1997)
    In:  Other Sources
    Details
    Publication Date: 2011-08-23
    Description: In this paper multiwavelength observations of an impulsive flare of May 9, 1991 are presented. This event was observed with the 48 GHz multibeam focal array used at the Itapetinga radio telescope, the microwave patrol telescopes at Bem and the BATSE high time resolution hard X-ray spectrometer on board CGRO. While spatially unresolved low sensitivity observations show two major impulsive peaks, the mm-wave observations with the ability of spatially high resolved tracking of the emission centroids suggest a primarily bipolar source configuration. For the first time two mm-wave sources with a spacing below the HPBW could be separated with the multibeam technique. The general features of the observations are explained as emission of partially trapped electrons. Furthermore we present evidence for highly inhomogeneous substructures within one of the two mm-wave sources for which the positional scatter of the emission center, within 2s, is less than 2".
    Keywords: Solar Physics
    Type: Astronomy and Astrophysics; Volume 317; 232-243
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  • 2
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    The rotation period of Uranus (1986)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: On 24 January 1986 the spacecraft Voyager 2 transversed the innermost magnetosphere of the planet Uranus, coming as close as 4.2 Uranus radii to the planet. It is pointed out that the magnetic field data provide a direct measure of the rotation period of the planet's interior, where the field is generated. Two period determinations are reported. A combination of the obtained values provides a weighted mean value of P = 17.24 + or - 0.01 h. It is concluded that the 17.24-h rotation period has important consequences for studies of atmospheric dynamics and the internal structure and composition of Uranus. Thus, inferences regarding the internal structure can be drawn from the relationship between the observed planetary oblateness, rotation period, and gravitational moment.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Nature (ISSN 0028-0836); 322; 42
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  • 3
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    Implications of the VEGA balloon results for Venus atmospheric dynamics (1986)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: Both VEGA balloons encountered vertical winds with typical velocities of 1 to 2 meters per second. These values are consistent with those estimated from mixing length theory of thermal convection. However, small-scale temperature fluctuations for each balloon were sometimes larger than predicted. The approximate 6.5-kelvin difference in temperature consistently seen between VEGA-1 and VEGA-2 is probably due to synoptic or planetary-scale nonaxisymmetric disturbances that propagate westward with respect to the planet. There is also evidence from Doppler data for the existence of solar-fixed nonaxisymmetric motions that may be thermal tides. Surface topography may influence atmospheric motions experienced by the VEGA-2 balloon.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Science (ISSN 0036-8075); 231; 1422-142
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  • 4
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    The magnetic field of Uranus (1987)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Aspherical harmonic model of the planetary magnetic field of Uranus is obtained from the Voyager 2 encounter observations using generalized inverse techniques which allow partial solutions to complex (underdetermined) problems. The Goddard Space Flight Center 'Q3' model is characterized by a large dipole tilt (58.6 deg) relative to the rotation axis, a dipole moment of 0.228 G R(Uranus radii cubed) and an unusually large quadrupole moment. Characteristics of this complex model magnetic field are illustrated using contour maps of the field on the planet's surface and discussed in the context of possible dynamo generation in the relatively poorly conducting 'ice' mantle.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research (ISSN 0148-0227); 92; 15329-15
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  • 5
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    Implications of preliminary Vega balloon results for the Venus atmosphere dynamics (1986)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The typical 1-2 m/sec vertical winds encountered by the Vega balloons probably result from thermal convection. The consistent 6.5-kelvin differential between the Vega 1 and Vega 2 temperatures is attributable to disturbances of synoptic or planetary scale. According to the Doppler tracking the winds were stronger than on earlier missions, perhaps because of solar thermal tides. The motions of Vega 2 may have been affected by waves from mountainous terrain.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Soviet Astronomy Letters (ISSN 0360-0327); 12; 22-25
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  • 6
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    Meteorological data along the Vega 1, 2 float paths (1986)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: The Vega balloons transmitted in situ measurements of pressure, temperature, vertical wind velocity relative to the balloon craft, cloud-particle backscatter coefficient, and ambient light level in the Venus middle cloud layer. Doppler tracking has yielded estimates for the velocities of atmospheric motion.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Soviet Astronomy Letters (ISSN 0360-0327); 12; 12-15
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  • 7
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    The Vega balloon experiments (1986)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The goals of the Vega-1 and -2 experiments were to trace the large- and small-scale motions, measure the turbulent heat and momentum flow in the cloud layer, and determine the physical parameters of the Venus atmosphere. The arrangement of the balloon-probe payload, the balloon-deployment sequence, and the balloon flight paths are described. The balloons drifted latitudinally in the Venus atmosphere about one-third the way around the planet at a height of 53-54 km and speeds close to 67 m/sec. The balloon-probe signals, recorded on earth by radio telescopes of ten countries, are being processed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Soviet Astronomy Letters (ISSN 0360-0327); 12; 3-5
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  • 8
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    Magnetic connection for Saturn's rings and atmosphere (1986)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Latitudinal variations in images of Saturn's disk, upper atmospheric temperatures, and ionospheric electron densities are found in magnetic conjugacy with features in Saturn's ring plane. It is proposed that these latitudinal variations are the result of a variable influx of water transported along magnetic field lines from sources in Saturn's ring plane. These features are thus the surface expression of an electromagnetic erosion mechanism which transports water (in the form of high charge-to-mass ratio particles) from the rings to the atmosphere.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Geophysical Research Letters (ISSN 0094-8276); 13; 773-776
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  • 9
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    Radio-interferometric imaging of the subsurface emissions from the planet Mercury (1987)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: The distribution of total and polarized intensities from Mercury's subsurface layers have been mapped using VLA observations. The first detection of a hot pole along the Hermean equator is reported and modeled as black-body reradiation from preferential diurnal heating. These observations appear to rule out any internal sources of heat within Mercury. Polarized emission from the limb of the planet is also found, and is understood in terms of the dielectric properties of the Hermean surface.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Nature (ISSN 0028-0836); 329; 224-226
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  • 10
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    The magnetospheres of Jupiter, Saturn, and Uranus (1987)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: The results published by U.S. scientists during 1983-1986 from studies related to the magnetospheres of Jupiter, Saturn, and Uranus are discussed. Consideration is given to the magnetic fields of these planets, charged particle environments, the interactions between the planetary rings and planetary satellites, the solar wind interactions, radio emissions, and auroras. Special attention is given to observations of (1) a small flux of energetic electrons and protons in the otherwise radiation-free environment in the magnetosphere under the rings of Saturn (interpreted as interactions of Galactic cosmic rays with the rings), (2) spokes, and (3) Saturn ring erosion.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Reviews of Geophysics (ISSN 8755-1209); 25; 615-638
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