Results 161 to 170 of about 698 (200)

On the Inclination Distribution of the Jovian Irregular Satellites

Icarus, 2002
Irregular satellites—moons that occupy large orbits of significant eccentricity e and/or inclination I—circle each of the giant planets. The irregulars often extend close to the orbital stability limit, about 1/3–1/2 of the way to the edge of their planet's Hill sphere. The distant, elongated, and inclined orbits suggest capture, which presumably would
V Carruba, Joseph A Burns, Philip D Nicholson   +2 more
exaly   +2 more sources

Jovian satellite nomenclature

Icarus, 1976
A brief review of the history of Jovian satellite nomenclature is given to indicate the background for the names proposed for the numbered satellites. The new names are consistent with established tradition and should cause minimal confusion with other named objects in the solar system.
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Filamentation of Volcanic Plumes on the Jovian Satellite IO

Astrophysics and Space Science, 1988
Volcanic plumes on the Jovian satellite Io may be a visible manifestation of a plasma-arc discharge phenomenon. The amount of power in the plasma arc (~ 1011 W) is not enough to account for all the energy dissipated by the volcanoes. However, once a volcano is initiated by tidal and geologic processes, the dynamics of the volcanic plumes can be ...
Anthony L. Peratt, A. J. Dessler
openaire   +1 more source

Thermal history of the Jovian satellite Io

Icarus, 1987
Abstract The discovery of large volcanic eruptions on Io suggests that Io is one of the most geologically active planetary bodies. The energy source of this geologic activity is believed to be tidal heating induced by Jupiter. A number of thermal history calculations were done to investigate the effect of tidal heating on the thermal history of Io ...
Shin-Ichi Kawakami, Hitoshi Mizutani
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Jovian and Saturnian satellites

Reviews of Geophysics, 1987
The years 1983‐1987 follow mankind's epochal first spacecraft encounters with the giant planets Jupiter and Saturn. Possibly the most spectacular “discoveries” there were the diversity and level of geological activity on the satellites that circle each.
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Jovian satellite-satellite eclipses and occultations

Icarus, 1973
Toward the end of 1973 and in the first part of 1974, when the planes of the orbits of the four large Galilean satellites cross the sun and the earth, satellite-satellite eclipses and occultations will occur. Calculations indicate that during this period 350 such events will occur, most of them potentially observable. From observation of a few of these
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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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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 ...
Roc M Cutrì, Robert H Hurt
exaly   +2 more sources

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
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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