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Ejecta types on Ganymede and Callisto

Ejecta types on Ganymede and Callisto have been identified from Voyager 1 and 2 images. Image resolution used range from approx. 0.6 to approx. 4 km/pxl, which allowed the surveying of almost all of the mappable surface of the two satellites. Seven ejecta classes were identified on Voyager images of Ganymede on the basis of albedo pattern and type of terminus. The ejecta of different terrains on ejecta characteristics were investigated for the most populated ejecta types. Two major ejecta types were identified on Callisto; both have counterparts on Ganymede. Type C1 has a uniformly high albedo and a sharp terminus. Type C2 has a gradational terminus and a moderate albedo. The similarity in ejecta types on Ganymede and Callisto may indicate similarities in the near surface environment of the two satellites, with different ejecta types representing several possible conditions for the impact environment.

Horner, V. M.↗

Ice and minerals on Callisto - A reassessment of the reflectance spectra

The results of a comparison of laboratory spectral reflectance measurements of particulate mixtures of both hydrated silicates and palagonite with water ice, on the one hand, with two previously unpublished reflectance spectra of Callisto, yield direct support for the hypothesis that the measured reflectance of Callisto includes a substantial nonice component. Hapke's (1981) equations are used in a theoretical model for thorough analysis of telescopic data; a comparison of the calculation results thus obtained with measured reflectance data for Callisto indicate that three-component, ice/magnetite/serpentine mixtures are a better match for telescopic data than two-component ice mixtures.

Roush, T. L.↗

Estimates of Comet Fragment Masses from Impact Crater Chains on Callisto and Ganymede

Chains of impact craters, or catenae, have been identified in Voyager images of Callisto and Ganymede. Although these resemble in some respects secondary crater chains, the source craters and basins for the catenae cannot be identified. The best explanation is a phenomenon similar to that displayed by former comet Shoemaker-Levy 9; tidal (or other) breakup close to Jupiter followed by gradual orbital separation of the fragments and collision with a Galilean satellite on the outbound leg of the trajectory. Because the trajectories must pass close to Jupiter, this constrains the impact geometry (velocity and impact angle) of the individual fragments. For the dominant classes of impactors, short period Jupiter-family comets and asteroids, velocities at Callisto and Ganymede are dominated by Jovian gravity and a satellite's orbital motion, and are insensitive to the pre-fragmentation heliocentric velocity; velocities are insensitive to satellite gravity for all impactor classes. Complex crater shapes on Callisto and Ganymede are determined from Voyager images and Schmidt-Holsapple scaling is used to back out individual fragment masses. We find that comet fragment radii are generally less than about 500 m (for ice densities) but can be larger. These estimates can be compared with those for the Shoemaker-Levy 9 impactors.

McKinnon, William B.↗

Plasma Densities in the Vicinity of Callisto from Galileo Plasma Wave Observations

The Galileo spacecraft has made seven close flybys of Jupiter's moon Callisto. During the closest of these (C22), which approached to within 535 km of the surface, the plasma wave instrument detected a very clear upper hybrid emission as the spacecraft passed near the moon. The peak electron density indicated by the upper hybrid resonance emission was 400/cc, almost one-thousand times the, electron density in the magnetosphere of Jupiter at the orbit of Callisto. These observations indicate that Callisto is probably surrounded by a dense ionospheric-like plasma.

Gurnett, D. A.↗

Geology of Lofn Crater, Callisto

Lofn crater is a 180-km-diameter impact structure in the southern cratered plains of Callisto and is among the youngest features seen on the surface. The Lofn area was imaged by the Galileo spacecraft at regional-scale resolutions (875 m/pixel), which enable the general geology to be investigated. The morphology of Lofn crater suggests that (1) it is a class of impact structure intermediate between complex craters and palimpsests or (2) it formed by the impact of a projectile which fragmented before reaching the surface, resulting in a shallow crater (even for Callisto). The asymmetric pattern of the rim and ejecta deposits suggests that the impactor entered at a low angle from the northwest. The albedo and other characteristics of the ejecta deposits from Lofn also provide insight into the properties of the icy lithosphere and subsurface configuration at the time of impact. The "target" for the Lofn impact is inferred to have included layered materials associated with the Adlinda multiring structure northwest of Loh and ejecta deposits from the Heimdall crater area to the southeast. The Lofn impact might have penetrated through these materials into a viscous substrate of ductile ice or possibly liquid water. This interpretation is consistent with models of the current interior of Callisto based on geophysical information obtained from the Galileo spacecraft.

Greeley, Ronald↗

The Pinnacles of Callisto

Many regions of Callisto feature an unusual landscape consisting of rolling dark plains with interspersed bright knobs (pinnacles) and ridges. In earlier work we interpreted the dark plains as dusty, mass-wasted residue from sublimation from volatile-rich bedrock and the bright knobs (often crater rims) as water ice accumulations at locations sheltered from thermal reradiation from the dusty residue. We simulated evolution of Callisto's craters as a combination of bedrock volatile sublimation, mass wasting of the dark, non-coherent residue, and redeposition of ice, and concluded that the ice pinnacles and ridges might be underlain by tens to hundreds of meters of ice. Here we report the initial work of a new study of pinnacles addressing additional questions: 1) Is there an evolutionary sequence starting, e.g., from a cratered initial surface through growth and formation of a dust mantle and pinnacles, to eventual loss of ice to sublimation resulting in just a dark, dusty surface? 2) What determines the areal density and spatial scale of pinnacles - volatile content of bedrock, crater density, surface age, broad-scale topographic setting? 3) Are pinnacles still forming? Several observations address these questions. In a few places scattered high-albedo blocks approx. 25-60 m in diameter occur in the vicinity of large icy pinnacles. We interpret these blocks to be remnants from the collapse of tall pinnacles that were undermined by mass wasting. Some high-relief icy knobs have developed a skeletonized planform due to mass wasting by avalanching, or perhaps to seeding of new sites of ice deposition on mass-wasted ice blocks. Some areas nearly lack fresh craters with well-defined ejecta and ice-free rims. This may imply rapid transformation of fresh craters by sublimation, mass wasting, and ice reprecipitation. In other areas small sharp-rimmed craters occur which lack ice pinnacles, but the craters nonetheless lack visible ejecta sheets. Our preliminary interpretation is that mass wasting is very efficient on Callisto, or alternatively the dust cover is very thick and lacks competent coarse materials.

bedrock volatile sublimation↗

Selection of an effective architecture for a precursor mission to Callisto

SAE 2003-01-2430This paper delineates an efficient and effective potential precursor mission architecture for making critical science measurements, and establishing sufficient infrastructure to facilitate human landing on Callisto. For orbiting, landing, and exploring the Callisto surface, the study addresses the problem of determining the tradeoff space in terms of hardware choices: monolithic, a large number of small, dexterous robotic, and their judicious combinations.

Callisto↗

Callisto - Disk temperature at 3.71-centimeter wavelength

We observed the radio emission of Callisto with a three-element interferometer at the time of the 1973 opposition of Jupiter. Special care was taken to remove the residual, unresolved contribution from Jupiter itself in the antenna side lobes. The resulting disk temperature at a wavelength of 3.71 centimeters, assuming a radius of 2500 + or - 75 kilometers for Callisto, was 101 + or - 25 K. This temperature is much more consistent with emission from a simple dielectric sphere than the considerably higher temperatures that have been reported for wavelengths of 3.5 and 8.2 millimeters.

Berge, G. L.↗

Identification of water frost on Callisto

A description is presented of broadband (J, K, and L) and narrowband (3.0-3.8 micrometers) observations of Ganymede and Callisto which were made on the nights of November 7 and November 29, 1976 with a 28-inch infrared telescope. Based on the previous identification of water frost on the surface of Ganymede from shorter wavelength data, it is concluded that there is also water frost on the surface of Callisto, taking into account the presence of similar bands for both satellites in the spectral range from 3 to 4 micrometers.

Lebofsky, L. A.↗

Internal processes affecting surfaces of low-density satellites - Ganymede and Callisto

Possible significant physical processes on low-density (icy) satellites, particularly Ganymede and Callisto, are outlined, and the relations of these interior processes to the formation and evolution of satellite surfaces are discussed. A variety of mechanisms is shown to lead to interior melting in early satellite history and a configuration characterized by a predominantly water ice lithosphere overlying a mantle containing liquid water. Physical processes capable of affecting the lithosphere of an ice-silicate body and thus creating observable surface features are assessed, including tectonic stresses from tidal deformation and volume changes, gravitational effects on density differences and water volcanism. The residence time of surface features on icy bodies produced by the outlined processes and by impact cratering is considered, and a tentative outline of the geologic history of Ganymede and Callisto is presented. Observations from Voyager and Galileo are expected to provide evidence on the evolution and geologic history of low-density satellites.

Parmentier, E. M.↗

The 16- to 38-micron spectrum of Callisto

The emission spectrum of Callisto was measured between 16 and 38 microns with a spectral resolution of 1/30 of a wavelength, using the NASA Kuiper Airborne Observatory on the night of October 30-31, 1975. Within the errors, the observed spectrum is like that of a 155 K blackbody, in both shape and absolute intensity. The infrared emission and diameter of Callisto indicate a bolometric Bond albedo of 0.05 + or - 0.14, which is consistent with heating of the surface by absorbed sunlight.

Forrest, W. J.↗

Volume changes in Ganymede and Callisto and the origin of grooved terrain

Internal melting and differentiation of Ganymede and Callisto may have caused an increase in the surface area of these bodies early in their histories of up to 5-7%. Subsequent refreezing of internal liquid water due to solid state convection in an ice crust should not have caused significant surface area changes. Expansion due to differentiation may have caused formation of grooved terrain in Ganymede. These calculations suggest that grooved terrain formation is essentially a replacement and/or deformation process, with no more than about 15% of grooved terrain actually being new material. The absence of grooved terrain on Callisto may be due to the effects of a thicker crust and a lower expansion rate.

Squyres, S. W.↗

Ganymede, Europa, Callisto, and Saturn's rings - Compositional analysis from reflectance spectroscopy

The reflectance spectra of Ganymede, Europa, Callisto, and the rings of Saturn are analyzed, using laboratory reflectance studies of water, frost, ice, and mineral mixtures. It is found that the spectra of the icy Galilean satellites are characteristic of water ice, or frost on ice, rather than pure water frost; and that the decrease in reflectance at visible wavelengths is caused by other mineral grains on the surface. The spectra of Saturn's rings are more characteristic of water frost, with other mineral grains mixed in the frost but not on the surface. It is also found that impurities of all these objects are not in isolated patches, but intimately mixed with the water. A new absorption feature at 1.15 microns has been identified in Ganymede, Callisto, and possibly Europa, which cannot be seen in Saturn's rings and whose cause is unknown.

Clark, R. N.↗

Evolution of planetary lithospheres - Evidence from multiringed structures on Ganymede and Callisto

The thickness and viscosity of a planetary lithosphere increase with time as the mantle cools, with a thicker lithosphere leading to the formation of one (or very few) irregular normal faults concentric to the crater. Since a gravity wave or tsunami induced by impact into a liquid mantle would result in both radial and concentric extension features, which are not observed in the case of the large impact structures on Ganymede and Callisto, an alternative mechanism is proposed in which the varying ice/silicate ratios, tectonic histories, and erosional mechanisms of the two bodies are considered to explain the subtle differences in thin lithosphere ring morphology between Ganymede and Callisto. It is concluded that the present lithosphere thickness of Ganymede is too great to permit the development of any rings.

Mckinnon, W. B.↗

Limits on large-crater production and obliteration on Callisto

By comparing results of Monte Carlo simulations of the crater population on Callisto with the observed surface, it is demonstrated that the relative dearth of large craters on Ganymede and Callisto, compared with the terrestrial planets, can not be totally ascribed either to craters relaxing or to craters piercing a thin icy crust. Consequently, the population of objects responsible for the heavy bombardment of the Jovian system differed markedly from that responsible for the late heavy bombardment of the terrestrial planets.

Woronow, A.↗

Thermal evolution of Ganymede and Callisto - Effects of solid-state convection and constraints from Voyager imagery

The imaging experiments of the Voyager 1 and 2 fly-by missions have provided a large amount of information about the nature of the surfaces of the Galilean satellites. The present investigation is concerned with the development of models regarding the thermal evolution of Ganymede and Callisto, taking into account the approach of parameterized convection. Attention is given to the physical, chemical, and geological data which are available as constraints on the thermal evolution of Ganymede and Callisto. Both satellites appear to possess surfaces composed of silicates and ice. However, their surface features are distinctly different from each other. In the discussion of thermal evolution models, attention is given to ice-dominant rheology, silicate-dominant rheology, and aspects of phase changes and solid-state convection.

Thurber, C. H.↗

Ripple Ring Basins on Ganymede and Callisto

The unusual morphology of the Valhalla multiple or ripple-ring basin in Callisto was totally unexpected in light of the morphologies of large impact structures on the terrestrial planets. Two other ripple-ring basins (RRB's), Asgard and a smaller structure near the crater Adlinda are also described. Several additional RRB's were found on Callisto, an example of which is shown. A previously unrecognized RRB on Ganymede was also found. An image and geologic sketch map of this RRB are shown. Morphometric and positional data for all known RRB's are given.

Croft, S. K.↗

Pionener 11 observations of effects of Ganymede and Callisto on Jupiter's trapped radiation

Charged particle data for low-energy protons and electrons from the Pioneer 11 high-latitude flyby of Jupiter in 1974 are reviewed in the light of the Voyager 1 magnetic field model of Connerney et al. (1981). It is found that if the trajectory of Pioneer 11 is mapped to the equatorial plane along the model magnetic field lines, significant features in the time-intensity profiles of trapped protons and electrons, including one microsignaturelike feature, are found to correspond to shells of closed field lines crossed by the orbits of Ganymede and Callisto. It is suggested that these features are signatures of interaction of the trapped particles with Ganymede and Callisto.

Mckibben, R. B.↗