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  • Lunar and Planetary Science and Exploration  (156)
  • 1
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    Microsat and Lunar-Based Imaging of Radio Bursts (2005)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: No present or approved spacecraft mission has the capability to provide high angular resolution imaging of solar or magnetospheric radio bursts or of the celestial sphere at frequencies below the ionospheric cutoff. Here, we describe a MIDEX-class mission to perform such imaging in the frequency range approx. 30 kHz to 15 MHz. This mission, the Solar Imaging Radio Array (SIRA), is solar and exploration-oriented, with emphasis on improved understanding and application of radio bursts associated with solar energetic particle (SEP) events and on tracking shocks and other components of coronal mass ejections (CMEs). SIRA will require 12 to 16 micro-satellites to establish a sufficient number of baselines with separations on the order of kilometers. The constellation consists of microsats located quasi-randomly on a spherical shell, initially of approx. 10 km diameter. The baseline microsat is 3-axis stabilized with body-mounted solar arrays and an articulated, earth pointing high gain antenna. The constellation will likely be placed at L1, which is the preferred location for full-time solar observations. We also discuss briefly follow-on missions that would be lunar-based with of order 10,000 dipole antennas.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Planetary Radion Emissions 6th; Apr 20, 2005 - Apr 22, 2005; Graz; Austria
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    NASA TECHNICAL REPORTS
  • 2
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    Lava Flows on Io: Modelling Cooling After Solidification (2003)
    In:  CASI
    Details
    Publication Date: 2017-10-02
    Description: We have modeled the cooling of lava bodies on Io after solidification of the lava, a process that has been little explored since Carr (1986). With recent estimates of lava flow thicknesses on Io ranging from 1 m to 10 m, the modeling of thermal emission from active volcanism must take into account the cooling behaviour after the solidification of the lava, which we model using a finite-element model. Once a lava body is fully solidified, the surface temperature decreases faster, as heat loss is no longer buffered by release of latent heat. This is significant as observed surface temperature is often the only clue available to determine lava surface age. We also find that cooling from the base of the lava is an important process that accelerates the solidification of a flow and therefore subsequent cooling. It is necessary to constrain the cooling process in order to better understand temperature-area relationships on Io's surface and to carry out stochastic modelling of lava flow emplacement.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXIV; LPI-Contrib-1156
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  • 3
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    Myriads of Small, Hot Eruptions on Io (2000)
    In:  Other Sources
    Details
    Publication Date: 2017-10-02
    Description: Should events such as the Tvashar fire fountain be expected? Examination of the Galileo Near Infrared Mapping Spectrometer (NIMS) C3 data set shows that the chances of observing some level of active volcanism in any given area covering at least 135 km(exp 2) is quite reasonable.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXI; LPI-Contrib-1000
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  • 4
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    Implication of the January 1990 Volcanic Eruption on Io for Resurfacing Rates and Energetics (1993)
    In:  Other Sources
    Details
    Publication Date: 2018-06-08
    Description: The high temperature event observed by ground based infrared radiometry of Io in January of 1990 can be modeled as an extremely active silicate lava flow which increased its area and cooled over a period of three hours. The best model at the start of the observations is a thermal source at 1200 K with an area equal to that of a circle of 5.6 km radius, while at the end of the observation sequence a source with a temperature of 700 K and a 13 km radium provides the best match. Given a flow thickness of 10 m, this implies an eruption rate of 300,000 cubic meters per second. This is large by terrestrial standards but consistent with estimates of lunar eruption rates (Head and Wilson 1981) and some terrestrial eruptions such as the 1800-1801 Hualalai flow in Hawaii (Baloga and Spudis 1992)...
    Keywords: Lunar and Planetary Science and Exploration
    Type: American Geophysical Union, Fall Meeting; San Francisco, CA; United States
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  • 5
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    Polar Heat Flow on Io (2003)
    In:  CASI
    Details
    Publication Date: 2017-10-02
    Description: Recently, Galileo spacecraft data have revealed Io's polar regions to be much warmer than previously expected. This unexpected development came from Photo-Polarimeter Radiometer (PPR) data which show that the minimum night temperatures are in the range of 90-95 K virtually everywhere on Io. The minimum night temperatures show no dependence upon latitude and, when away from the sunset terminator, they show no dependence upon time of night. This is indeed bizarre behavior for surface units which generally had been assumed to be passive with respect to Io's pervasive volcanism. Night temperatures of 90-95 K at high, polar latitudes are particularly hard to explain. Even assuming infinite thermal inertia, at these latitudes there is insufficient sunlight to support these warm night temperatures. Thus, through the process of elimination of other possibilities, we come to the conclusion that these surfaces are volcanically heated. Taking previously passive units and turning them into new sources of heat flow is a radical departure from previous thermophysical model paradigms. However, the geological interpretation is straight forward. We are simply seeing the effect of old, cool lava flows which cover most of the surface of Io but yet have some heat to radiate. Under these new constraints, we have taken on the challenge of formulating a physical model which quantitatively reproduces all of the observations of Io's thermal emission. In the following we introduce a new parametric model which suffices to identify a previously unrecognized polar component of Io's heat flow.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXIV; LPI-Contrib-1156
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  • 6
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    Io's Volcanism: Similarities and Differences with the Earth and Moon (1997)
    In:  Other Sources
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    Publication Date: 2018-06-08
    Keywords: Lunar and Planetary Science and Exploration
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  • 7
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    Joint Galileo/ Cassini observations of the Jovian system (2001)
    In:  Other Sources
    Details
    Publication Date: 2018-06-08
    Keywords: Lunar and Planetary Science and Exploration
    Type: The Geological Society of America Cordilleran Section - 97th Annual Meeting; Universal City, CA; United States
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  • 8
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    Io: Heat Flow and Surface Age (2001)
    In:  Other Sources
    Details
    Publication Date: 2019-08-17
    Description: Assuming Io is completely resurfaced with volcanics, ages to surface units on Io can be assigned as a function of temperature. Additional information is contained in the original extended abstract.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXII; LPI-Contrib-1080
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  • 9
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    The Mystery of Io's Warm Polar Regions: Implications for Heat Flow (2002)
    In:  Other Sources
    Details
    Publication Date: 2019-08-15
    Description: Unexpectedly warm polar temperatures further support the idea that Io is covered virtually everywhere by cooling lava flows. This implies a new heat flow component. Io's heat flow remains constrained between a lower bound of (approximately) 2.5 W m(exp -2) and an upper bound of (approximately) 13 W m(exp -2). Additional information is contained in the original extended abstract.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXIII; LPI-Contrib-1109
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  • 10
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    Hydrogen peroxide on the surface of Europa (1999)
    In:  Other Sources
    Details
    Publication Date: 2011-08-24
    Description: Spatially resolved infrared and ultraviolet wavelength spectra of Europa's leading, anti-jovian quadrant observed from the Galileo spacecraft show absorption features resulting from hydrogen peroxide. Comparisons with laboratory measurements indicate surface hydrogen peroxide concentrations of about 0.13 percent, by number, relative to water ice. The inferred abundance is consistent with radiolytic production of hydrogen peroxide by intense energetic particle bombardment and demonstrates that Europa's surface chemistry is dominated by radiolysis.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science (ISSN 0036-8075); Volume 283; 5410; 2062-4
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