Results 161 to 170 of about 140,689 (193)

Another 'Ocean' for a Jovian Satellite?

Science, 1999
PLANETARY SCIENCEObservations from the ground and the Galileo spacecraft suggest the existence of an ocean on the fiery Jovian satellite Io. But there are no tantalizing prospects for life in Io's proposed ocean. At something like 2000 Kelvin, the ocean seething beneath Io's volcanoes and lava lakes would vaporize the hardiest creature, for this ocean ...
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Origin of the Different Architectures of the Jovian and Saturnian Satellite Systems [PDF]

Astrophysical Journal, 2010
The Jovian regular satellite system mainly consists of four Galilean satellites that have similar masses and are trapped in mutual mean motion resonances except for the outer satellite, Callisto. On the other hand, the Saturnian regular satellite system has only one big icy body, Titan, and a population of much smaller icy moons.
Sasaki, Takanori, Stewart, Glen R., Ida, Shigeru   +2 more
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Near-Infrared Observations of the Outer Jovian Satellites

Icarus, 2000
Abstract On September 21, 1998, the outer jovian satellites Himalia (J6), Elara (J7), Carme (J11), Pasiphae (J8), and Sinope (J9) were detected in the J , H , and K s bandpasses in the course of the Two-Micron All Sky Survey. Similarities in near-infrared colors are consistent with the hypothesis that the outer satellites in prograde orbits are ...
Michael F. Skrutskie, Mark V. Sykes
exaly   +2 more sources

Origin of the jovian ring and the galilean satellites

Nature, 1979
THE discovery by Voyager I of a thin flat stream of rocks orbiting Jupiter at a radius of some 130,000 km, or ∼2RP (Rp = 6.677 × 109 cm = present polar radius), in its equatorial plane opens a new avenue of information in our understanding of the formation of the Solar System.
A. J. R. PRENTICE, D. TER HAAR
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Mutual phenomena of Jovian satellites

Journal of Astrophysics and Astronomy, 1991
Results of the observations of mutual eclipses of Galilean satellites observed from the Vainu Bappu Observatory during 1985 are presented. Theoretical models assuming a uniform disc, Lambert’s law and Lommel-Seeliger’s law describing the scattering characteristics of the surface of the eclipsed satellite were used to fit the observations.
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1979J2: The Discovery of a Previously Unknown Jovian Satellite

Science, 1980
During a detailed examination of imaging data taken by the Voyager 1 spacecraft within 4.5 hours of its closest approach to Jupiter, a shadow-like image was observed on the bright disk of the planet in two consecutive wide-angle frames. Analysis of the motion of the image on the Jovian disk proved that it was not an atmospheric feature ...
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The galilean satellites and the Jovian magnetic field

The Moon and the Planets, 1978
Alfven and Arrhenius (1974, 1976) have proposed that satellites may be formed by the condensation of plasma in partial corrotation in the dipole magnetic field of the central body. They conclude that the final orbit distance of the condensed material will be two-thirds of the orbit distance of the plasma.
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Galilean Satellites and Jovian Energetic Particles

Science, 1975
The observed infrared temperatures of the four Galilean satellites, Io, Europa, Ganymede, and Callisto, are inconsistent with their equilibrium temperatures. Since these satellites appear to have little or no atmosphere, the discrepancies may be explained as due to the heating of their surfaces by energetic particles from Jupiter's radiation belts. The
exaly   +2 more sources

An evolutionary framework for the Jovian and Saturnian satellites

Earth, Moon, and Planets, 1987
The position of the satellite within the protonebula, the influence of the parent planet, particularly the relative effects of tidal (gravitational) as opposed to radiogenic (internal) heat generating processes, as well as the type of ice, exert a control on the evolutionary histories of the Jovian and Saturnian satellites.
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The Icy Jovian Satellites After the Galileo Mission

Reports on Progress in Physics, 2010
The icy satellites of Jupiter, Callisto, Ganymede, Europa and Amalthea have diverse and remarkable characteristics. Their initial compositions were determined by conditions in the circum-Jovian nebula, just as the planets' initial properties were governed by their formation within the circumsolar nebula.
Richard Greenberg
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