The Imaging Photopolarimeter Experiment on Pioneer 10

Gehrels, T.; Coffeen, D. L.; Tomasko, M. G.; Doose, L. R.; Swindell, W.; Castillo, N. D.; Kendall, Joseph; Clements, Andy W.; Hämeen-Anttila, J.; Knight, Cynthia; Blenman, C.; Baker, Robert; Best, G. T.; Baker, L. R.

doi:10.1126/science.183.4122.318

Cited by 33 publications

(8 citation statements)

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“…A particularly perplexing problem has been the conflicting evidence of the Jovian NIt a abundance from infra-red and ultra-violet observational data. Interpretation of the ultra-violet data suggests an NIt 3 abundance 3 orders of magnitude less than that inferred from the infra-red data (Anderson et al 1969, Tomasko 1974. Since the infra-red radiation penetrates more deeply into the atmosphere than ultra-violet radiation it does not follow that the NH a abundances inferred from observations at these wavelengths should be similar.…”

Section: Instrumentmentioning

confidence: 64%

“…Tomasko et al (1974) estimate a Value of ~ 1.5 for the Jovian phase angle from the Pioneer 10 observations. I~ Saturn has a similar value for this parameter, then Rieke (1975) estimates an equilibrium temperature of 76 + 4K.…”

Section: Atmospheric Structurementioning

confidence: 99%

“…Ultra-violet photometer (Carlson and Judge 1974) Imaging photopolarimeter (Gehrels et al 1974) Infra-red radiometer (Chase et al, 1974) S-band occultation (Kliore et al, 1974) Objectives To investigate the hydrogen and helium emissions and determine the ratio of hydrogen to helium To determine cloud morphology shape, size and refractive index of cloud particles from measurements of polarization and intensity of reflected sunlight…”

Section: Instrumentmentioning

confidence: 99%

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The atmospheres of the outer planets

Hunt

1976

Advances in Physics

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Beyond the asteroid belt lie the giant planets, Jupiter, Saturn, Uranus and Neptune and their extensive satellite systems, and Pluto, which is more like a satellite than any of its giant companions. Those large planets are huge, rapidly rotating bodies and seem to Ibrm two separate families.Jupiter and Saturn appear to have an apparently permanently banded appearance of alternating light and dark clouds of rapidly changing colours. The composition of their atmospheres seems to be similar to that of the Sun. Present theories are unable to account for the banded structure, the origin of the colours and the Great Rod Spot situated in the southern Jovian hemisphere. These planets are surrounded by an extensive system of 23 satellites. Two of them, Io of the Galilean satellites, and Titan of the Saturnian system, have atmospheres. The Titan atmosphere is thought to be considerably larger than the present Martian atmosphere.Uranus and Neptune are thought to form a separate family of planets, with less than solar proportions of the light elements, and larger portions of methane than found on Jupiter and Saturn.In this article, which was completed in March 1976, we review our current understanding of the atmospheres of the major planets. CONTENTS

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Section: Instrumentmentioning

confidence: 64%

Section: Atmospheric Structurementioning

confidence: 99%

Section: Instrumentmentioning

confidence: 99%

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The atmospheres of the outer planets

Hunt

1976

Advances in Physics

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“…Pioneer pictures of Jupiter (see for example Gehrels et al, 1974;Baker et al, 1975) show many small light and dark spots along with small-scale wave disturbances. From these single pictures, however, it is not known whether these features are minor perturbations on the basic zonal structure or an essential part of it.…”

Section: Local Motionsmentioning

confidence: 97%

Voyager imaging experiment

et al. 1977

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Abstract. The overall objective of this experiment is exploratory reconnaissance of Jupiter, Saturn, their satellites, and Saturn's rings. Such reconnaissance, at resolutions and phase angles unobtainable from Earth, can be expected to provide much new data relevant to the atmospheric and/or surface properties of these bodies. The experiment also has the following specific objectives:Observe and characterize the global circulation of the atmospheres of Jupiter and Saturn; Determine the horizontal and vertical structure of the visible clouds and establish their relationship to the belted appearance and dynamical properties of the planetary atmospheres;Determine the vertical structure of high, optically-thin, scattering layers on Jupiter and Saturn; Determine the nature of anomalous features such as the Great Red Spot, South Equatorial Belt disturbances, etc.;Characterize the nature of the colored material in the clouds of Jupiter and Saturn, and identify the nature and sources of chromophores on Io and Titan;Perform comparative geologic studies of many satellites at less than 15-km resolution; Map and characterize the geologic structure of several satellites at high resolution (-1 kin); Investigate the existence and nature of atmospheres on the satellites;

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“…Moon, Vesta, and soon Ceres Lunar Orbiters High-resolution Hansen (1970) 1 to 10s Medium-resolution Hansen (1970) Jupiter's moons Pioneer 10 Imaging photopolarimeter experiment Gehrels et al (1974) 160,000-800,000 Pioneer 11…”

Section: Mercurymentioning

confidence: 99%

An introduction to the data and tools of planetary geomorphology

Beyer

2015

Geomorphology

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a b s t r a c tThis manuscript presents a review of data used by planetary geomorphologists and the software tools needed to prepare, process, and analyze those data, along with an example of doing so. Visible image capture and the photometric and geometric processing of those images are reviewed, as are laser altimetry data, and terrain data derived from images via stereogrammetry. Image processing, geographic, and geospatial software tools are discussed.

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The Imaging Photopolarimeter Experiment on Pioneer 10

Cited by 33 publications

References 1 publication

The atmospheres of the outer planets

The atmospheres of the outer planets

Voyager imaging experiment

An introduction to the data and tools of planetary geomorphology

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