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  • LUNAR AND PLANETARY EXPLORATION  (35)
  • Physics
  • 1990-1994  (35)
  • 1
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    Whistler mode waves in the Jovian magnetosheath (1994)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: During the Ulysses flyby of Jupiter in February 1992, the spacecraft traversed the Jovian magnetosheath for a few hours during the inbound pass and for aa few days during the outbound pass. Burstlike electomagnetic waves at frequencies of approximately 0.1-0.4 of the local electron cyclotron frequency have been observed by the Unified Radio and Plasma Wave (URAP) experiement. The waves were more often observed in the regions which were probably the outer or the middle magnetosheath, especially near the bow shock, and rarely seen in the magnetosphere/magnetosheath boundary layer. The propagation angles of the waves are estimated by comparing the measurements of the wave electric and magnetic fields in the spacecraft spin plane with the corresponding values calculated using the cold plasma dispersion relation under local field and plasma conditions. It is found that the waves propagate obliquely with wave angles between approximately 30 deg and 50 deg. These waves are likely to be the whistler mode waves which are excited by suprathermal electrons with a few hundred eV and a slight anisotropy (T(sub perp)/T(sub parallel) approximately 1.1-1.5). They are probably similar in nature to the lion roars observed in the Earth's magnetosheath. Signature of coupling between the mirror and the whistler mode have also been observed. The plasma conditions which favor the excitation of the whistler mode instability during the wave events exists as observed by the plasma experiement of Ulysses.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research (ISSN 0148-0227); 99; A12; p. 23,527-23,539
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  • 2
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    Recent high resolution laboratory determinations of line broadening and intensity parameters: PH3, CH3D, and CO2 (1990)
    In:  CASI
    Details
    Publication Date: 2016-06-07
    Description: Recent unpublished laboratory work on rovibrational line strengths and broadening coefficients which is of interest in the study of planetary atmospheres was reviewed. The molecules discussed are PH3, CH3D and CO2.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Goddard Space Flight Center, First International Conference on Laboratory Research for Planetary Atmospheres; p 74-77
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  • 3
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    Polar sediment accumulation: Role of surface winds at the two poles (1993)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: The accumulation of the large deposits of volatile and nonvolatile sediments at both Martian poles has occurred through periods of likely climate change. Most data on wind directions near the Martian poles and seasonal activity relate to a very short period of time, at one point in climate cycles. It is still uncertain what the net budgets to the poles are and how this budget (if known) would fit into longer climate/sediment cycles. Pending further data we examined the full suite of Viking high-resolution, high-latitude images for wind markers of all sizes and types. These probably represent timescales of formation from days to several tens of thousands of years. The goal is to estimate the effectiveness, and possible drivers, of wind systems that bring materials near the surface to the regions of polar sediments and that also remove materials from the polar areas.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Mars: Past, Present, and Future. Results from the MSATT Program, Part 1; p 49
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  • 4
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    Volcanism by melt-driven Rayleigh-Taylor instabilities and possible consequences of melting for admittance ratios on Venus (1992)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: A large number of volcanic features exist on Venus, ranging from tens of thousands of small domes to large shields and coronae. It is difficult to reconcile all these with an explanation involving deep mantle plumes, since a number of separate arguments lead to the conclusion that deep mantle plumes reaching the base of the lithosphere must exceed a certain size. In addition, the fraction of basal heating in Venus' mantle may be significantly lower than in Earth's mantle reducing the number of strong plumes from the core-mantle boundary. In three-dimensional convection simulations with mainly internal heating, weak, distributed upwellings are usually observed. We present an alternative mechanism for such volcanism, originally proposed for the Earth and for Venus, involving Rayleigh-Taylor instabilities driven by melt buoyancy, occurring spontaneously in partially or incipiently molten regions.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Papers Presented to the International Colloquium on Venus; p 123-124
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  • 5
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    Thermal structure and dynamics of Neptune's atmosphere from Voyager measurements (1991)
    In:  Other Sources
    Details
    Publication Date: 2011-08-24
    Description: The thermal structure of the Neptunian atmosphere between 50 and 10 mbar is characterized using spatially resolved Voyager IR spectra from a global mapping sequence. A zonal mean meridional temperature cross section was obtained which shows a minimum in the upper tropospheric and lower stratospheric temperatures at the southern mid-latitudes, and maxima at the equator and at high southern latitudes. This structure is qualitatively similar to the thermal structure of the Uranian atmosphere, even though the obliquities and the internal heat fluxes of the two planets are quite different.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research Supplement (ISSN 0148-0227); 96; 18
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  • 6
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    Chronology, eruption duration, and atmospheric contribution of Apollinaris Patera, Mars (1993)
    In:  Other Sources
    Details
    Publication Date: 2019-01-25
    Description: Geologic mapping from Viking image data of the Martian volcano Apollinaris Patera allowed identification of 6 major events that shaped its current morphology. Derivation of new topographic data allowed accurate estimates of the volume of erupted products from which estimates of an eruption duration are presented for the edifice and its corresponding atmospheric water contribution. Topographic data were acquired using stereophotogrammetric (Viking picnos 603A42, 639A92) techniques in both profiling and contouring modes (1 km contour). The profiling mode results in a more precise measurement than the contouring mode, but is limited in its areal coverage. The contour data are used in a more general sense to provide synoptic coverage for the volcano. These new stereophotogrammetric measurements constrain the topography to an accuracy of approximately 800 m vertically and approximately 1000 m horizontally. Conversion of the derived contour map to a raster based digital elevation model (DEM) was done by a growing contours interpolation. An ambiguity arises in this volume calculation due to an uncertainty regarding the actual base of the volcano relative to the pre-existing topography. Thus, the volume estimate was bracketed by using the 100 m and the 750 m elevations, which generally correspond to the lower and upper portions of the circumferential basal scarp, respectively. The resulting volumes are 103,000 cu km and 97,000 cu km; therefore the total volume of Apollinaris Patera is estimated to be approximately 100,000 cu km.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 3: N-Z; p 1209-1210
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  • 7
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    Depth/diameter relationships of fresh craters within Hesperia Planum, Mars (1991)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Meteorite impact craters represent important geological features for revealing the near-surface layers of a planetary surface. In the case of Mars, this characteristic was proposed as a useful method to study spatial variations of such attributes as the distribution of sub-surface volatiles, and heat flow. Using the Planetary Image Cartography System (PICS) software, a quantitative analysis was completed of the geometry of fresh impact craters in the Hesperia Planum region of Mars, where an uniform target material and optimum viewing geometry make possible an analysis of target effects over a large geographic region. Because of the morphologic similarity to the lunar maria, it is likely that Hesperia Planum comprises a series of flood lavas that partially infilled topographic depressions within the Martian highlands. Measurements of partially buried crater rims suggest that the lava flows within Hesperia Planum are between 200-400 m thick.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1990; p 370-372
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  • 8
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    New studies of Martian volcanoes (1991)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: To investigate the morphology, topography, and evolution of volcanic constructs on Mars, researchers have been studying the volcanoes Olympus Mons, Tyrrhena Patera, and Apollinaris Patera. These studies relied upon the analysis of digital Viking orbiter images to measure the depth and slopes of the summit area of Olympus Mons, upon new Earth-based radar measurements for the analysis of the slopes of Tyrrhena Patera, and upon the color characteristics of the flanks of Apollinaris Patera for information regarding surface properties.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1990; p 174-176
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  • 9
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    Valley systems on Tyrrhena Patera, Mars - Earth-based radar measurements of slopes (1992)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: The presently treated eight topographic profiles across the Martian volcano Tyrrhena Patera indicate that the vocano rises about 1.5 km above the plains of Hesperia Planum to the east, and exhibit an average height/diameter ratio of about 1:340. The slopes of the northern flank of Tyrrhena Patera bear little correlation with the width or depth of valley systems in that area, suggesting that erosion by gravity-driven flows was not responsible for valley formation. Attention is given to such other valley geometry and location controlling factors as ground-water release variations and volcano surface unit materials' strength differences.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Icarus (ISSN 0019-1035); 96; 2 Ap
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  • 10
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    Martian parent craters for the SNC meteorites (1992)
    In:  Other Sources
    Details
    Publication Date: 2019-08-28
    Description: Information on the petrology and ages of the SNC meteorites, together with geological data derived from Viking Orbiter images, are used to identify 25 candidate impact craters in the Tharsis region of Mars that could possibly be the source craters for these meteorites. The craters chosen as candidate source craters had diameters greater than 10 km, morphologies indicative of young craters, and satisfied both the petrological criteria of the SNCs and the proposed 1.3 Ga crystallization ages. On the basis of the constraints implied by the identification of the candidate source craters, interpretations of the absolute chronology of Mars are proposed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research (ISSN 0148-0227); 97; E6 J; 10
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