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  • 1985-1989  (7)
  • 1980-1984  (23)
  • 1970-1974  (3)
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  • 1
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    Infrared observations of planetary atmospheres (1986)
    In:  CASI
    Details
    Publication Date: 2006-02-14
    Description: Infrared data was obtained on planetary atmospheres which provides critical information on atmospheric structure, composition, and cloud properties in support of planetary missions such as Voyager and Galileo. Mapping of Jupiter and Saturn in thermal and reflected solar radiation is a high-priority monitoring and exploratory activity. Some of these images of Jupiter are shown. Radiation at 17.8 micrometer probes the upper tropospheric temperature structure where spatial structure bears a strong resemblance to visible and near-infrared reflected sunlight such as at 2.0 micrometer. At 7.8 micrometer, stratospheric temperatures appear to have a three-banded structure, enhancements near the magnetic poles and occasional transient features such as the equatorial filament near the right limb. Clouds or hazes are observed high in the stratosphere looking at wavelengths such as 2.2 micrometer, where gaseous opacity is very strong. Other maps examine cloud properties from thermal radiation not strongly influenced by gaseous opacity and the distribution of condensable gases, such as ammonia. Millimeter and submillimeter filtered radiometric observations were made of Jupiter, Uranus and Neptune via collaborative work. Radiometric observations of Uranus and Neptune at 21 and 32 micrometer were acquired and analyzed as well as grating array spectra in the ranges of 8 to 14 micrometer, 16 to 23 micrometer, and 18 to 32 micrometer. These showed evidence for C2H2 in the stratosphere of Uranus and C2H4 in the stratosphere of Neptune.
    Keywords: ASTRONOMY
    Type: NASA, Washington Reports of Planetary Astronomy, 1985; p 49-50
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  • 2
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    Far Infrared and Submillimeter Observations of the Giant Planets (1984)
    In:  CASI
    Details
    Publication Date: 2014-09-17
    Description: Far infrared measurements of the effective temperatures of Jupiter, Saturn, Uranus and Neptune were made. The measurements presented here cover the range from 35-1000 micrometers in relatively narrow bands. The observations at lambda 350 micrometers were made at the 3m NASA Infrared Telescope Facility (IRTF) of the Mauna Kea Observatory; those at lambda 350 micrometer were made on the Kuiper Airborne Observatory (KAO). All observations of Saturn were made when the ring inclination to Earth was 1.7 deg assuring an unambiguous measurement of the flux from the disk itself. Mars was used as the calibration reference. The results represent a consistent set of calibration standards. In these measurements, it is assumed that sub b(lambda = 350 micrometers) = T sub (lambda 350 micrometers). Measurements have been made of roughly 50% of the total flux emitted by Jupiter, 65% by Saturn, and 92% by Uranus and Neptune. These measurements therefore permit a considerable reduction in the uncertainties associated with the bolometric thermal outputs of the planets. The effective temperatures (T sub e) and the ratios of emitted to absorbed solar radiation were calculated.
    Keywords: ASTRONOMY
    Type: NASA. Ames Research Center Airborne Astron. Symp.; p 81-86
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  • 3
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    Pioneer Saturn infrared radiometer - Preliminary results (1980)
    In:  Other Sources
    Details
    Publication Date: 2011-08-17
    Description: Preliminary results of the infrared radiometer experiment on Pioneer Saturn are reported. The instrument made use of two broadband channels centered at 20 and 45 microns which scan at a fixed 75-deg angle with respect to the spacecraft spin axis to acquire 10,000 image pairs of Saturn and its rings in the 2.5 h before closest approach, as well as several observations of Titan. The intensities of radiation observed in both bands indicate an effective temperature of 94.4 + or - 3 K for the planet, implying a total emission greater than twice the absorbed sunlight. Infrared data also indicates a molecular abundance of 0.85 for H2 relative to H2 + He, which can be improved by comparing the derived temperature profiles and radio occultation data. Planetary temperatures are found to range from a minimum of 83 to 140 K at the 1 bar level, with differences of 2.5 K between belts and zones up to the 0.06-bar level, while ring temperatures range from 60 to 70 K on the illuminated side and from less than 60 to 67 K in the planet's shadow and average 55 K on the unilluminated side. Preliminary estimates indicate a 45-micron brightness temperature of 80 + or - 10 K for Titan.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Science; 207; Jan. 25
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  • 4
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    Saturn's atmospheric temperature structure and heat budget (1980)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: The effective temperature of Saturn from 30 deg S to 10 deg N is 96.5 + or - 2.5 K. This value is 1.9 K higher than a preliminary estimate (Ingersoll et al., 1980). The atmospheric mole fraction of H2 + He is 90 + or - 3%. This value is derived by comparing infrared and radio occultation data (Kliore et al., 1980) for the same latitude. The high value of the effective temperature suggests that Saturn has an additional energy source besides cooling and contraction. The high mole fraction of H2 suggests that separation of heavier He toward the core may be supplying the additional energy. Atmospheric temperatures in the 60- to 600-mbar range are 2.5 K lower within 7 deg of the equator than at higher latitudes. An almost isothermal layer exists between 60 and 160 mbar at all latitudes.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research; 85; Nov. 1
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  • 5
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    Scientific results from the Pioneer Saturn infrared radiometer (1981)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: Data on Saturn and its rings are presented, obtained by the Pioneer 11 infrared radiometer in broadband channels, centered at 20 and 45 microns. Assuming symmetry about the equator and a constant flux poleward of 7.5 deg latitude, an average effective temperature of 96.5 + or - 2.5 K indicates a total emission which is 2.8 times that of the absorbed sunlight. Temperatures at the 1 bar level are 137 and 140 K, and a minimum temperature averaging 87 K is registered near the 0.06 bar level. Ring boundaries and optical depths are consistent with those at optical wavelengths. Ring temperatures are 54-86 K on the south side, approximately 54 K on the north side, and at least 67 K in Saturn's shadow.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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  • 6
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    Far infrared and submillimeter brightness temperatures of the giant planets (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The brightness temperatures of Jupiter, Saturn, Uranus, and Neptune in the range 35 to 1000 micron. The effective temperatures derived from the measurements, supplemented by shorter wavelength Voyager data for Jupiter and Saturn, are 126.8 + or - 4.5 K, 93.4 + or - 3.3 K, 58.3 + or - 2.0 K, and 60.3 + or - 2.0 K, respectively. The implications of the measurements for bolometric output and for atmospheric structure and composition are discussed. The temperature spectrum of Jupiter shows a strong peak at approx. 350 microns followed by a deep valley at approx. 450 to 500 microns. Spectra derived from model atmospheres qualitatively reproduced these features but do not fit the data closely.
    Keywords: ASTRONOMY
    Type: NASA-TM-88179 , REPT-86003 , NAS 1.15:88179 , PREPRINT-SERIES-33
    Format: application/pdf
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  • 7
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    Thermal infrared constraints on ammonia ice particles as candidates for clouds in the atmosphere of Saturn (1983)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: Saturn atmosphere thermal IR emission observations have uncovered two phenomena that may be accounted for by large ammonia ice particles: the depression of thermal brightness near the equator, and inconsistent IR and radio occultation results. Ammonia ice particles yield the opacity that can account for the contrast between the equatorial region and a brighter area near 15 deg S, and may also reconcile the 45-micron brightness of these two regions with the mean temperature structure of Voyager 2 radio occultation results. A cloud model whose ice particles are distributed in an equal ratio with gas particles up to the 100 mbar pressure level is found to fit the equatorial data, while a thinner cloud, or one that does not extend higher than the 400 mbar limit of the convective region matches the 15 deg S data.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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  • 8
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    Temperature Structures and Infrared-Derived Properties of the Atmosphere of Uranus and Neptune (1984)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Temperature structures of Uranus and Neptune are currently derivable from a combination of stellar occultation and thermal radiance observations. The globally averaged temperatures of Uranus and Neptune appear quite similar in their convective regions, reaching temperatures near 75 K at 1 bar and 150 K near 10 bar. Temperature minima near 200 mbar are also similar, near 53 to 55 K. The temperature in the stratosphere of Neptune rises much more steeply with altitude than for Uranus in the range of 0.1 to 100 mbar. Above this level, near 1 ubar, both atmospheres reach temperatures of 120 to 160 K. The bolometric radiant energy output is equivalent to the output of a blackbody at 58.3 + or - 2.0 K for Uranus and 60.3 + or - 2.0 for Neptune. These values imply approximate equilibrium with absorbed sunlight for Uranus but an internal energy source 1.9 to 2.6 times the absorbed sunlight for Neptune. The implication of the thermal spectra is that while the bulk composition may be consistent with a solar mixture of H2 and He, the mixing ratio of CH4 is probably about 2% in the deep atmospheres of both planets.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Uranus and Neptune; p 89-156
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  • 9
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    New observational constraints on the temperature inversions of Uranus and Neptune (1983)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: The presence of a temperature inversion in the lower stratospheres of both Uranus and Neptune is confirmed by the 20-micron photometric data presented. It is found that the brightness temperature difference between 17.8 and 19.6 microns is 0.8 + or - 0.5 K for Uranus and 1.8 + or - 0.6 K for Neptune, implying that the temperature inversions of both planets are weaker than previously thought. Comparisons with model atmospheres suggested by Appleby (1980) imply that these temperature inversions may be understood as a consequence of heating through CH4 and aerosol absorption of sunlight. The stratospheric CH4 mixing ratio of Neptune must, however, be higher than that at the temperature minimum.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Icarus; 53; Jan. 198
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  • 10
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    Further observations of 8-micron polar brightenings of Jupiter (1983)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: North-to-south scans of Jupiter at 7.8-micron wavelength in early 1981 confirm polar brightening events that correlate with LCM (III), such that a polar limb is bright when the corresponding magnetic pole is tilted earthward. The correlation with magnetic features of the planet suggests that the energy source for the brightenings is magnetospheric particles incident upon the polar regions of the atmosphere. The northern polar events are more prominent and more regular than the southern ones. The polar emission may be indirectly related to the ultraviolet absorber observed near the poles by Voyager 2.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Icarus; 53; Jan. 198
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