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Mutual phenomena of Jovian satellites
Journal of Astrophysics and Astronomy, 1991Results 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, 1980During 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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Erosion of Galilean Satellite Surfaces by Jovian Magnetosphere Particles
Science, 1981The Galilean satellites of Jupiter—Io (J1), Europa (J2), Ganymede (J3), and Callisto (J4)—are embedded in the intense ion and electron fluxes of the Jovian magnetosphere. The effect of these particles on the icy surfaces of the outer three satellites depends on the fluxes and the efficiency of the sputtering of water ice by such particles.
R E, Johnson +3 more
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CCD photometry for Jovian eclipses of the Galilean satellites
Icarus, 1992Abstract Timings of nine Jovian eclipses of the Galilean satellites observed during 1990 and 1991 are compared to predictions from modern ephemerides and are shown to exhibit very little internal scatter. These data can be used to supplement astrometry from the mutual occultations and eclipses of the satellites that occurred during the same time ...
Anthony Mallama
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Galilean Satellites and Jovian Energetic Particles
Science, 1975The 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
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An evolutionary framework for the Jovian and Saturnian satellites
Earth, Moon, and Planets, 1987The 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 galilean satellites and the Jovian magnetic field
The Moon and the Planets, 1978Alfven 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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Regions of possible motions for new Jovian satellites
Solar System Research, 2007We present the results of our simulation and study of the regions of possible motions for 46 newly discovered Jovian satellites. We show that the orbits of some satellites (such as S/2003 J02, S/2003 J03, S/2003 J04, S/2003 J10, S/2003 J12, and S/2003 J23) presently cannot yet be determined with an acceptable accuracy for planning observations, because
V. A. Avdyushev, M. A. Banschikova
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The Jovian Irregular Satellites with MIRI LRS
The irregular satellites of Jupiter are a swarm of small, asteroid-like objects in orbit from ~100-400 Jupiter radii from the planet. These objects are thought to have been captured after the planet formed, although their precise origins remain obscure. Previous results have found the Jovian irregular satellites to contain a wide abundance of materials,Benjamin Sharkey +5 more
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The origin of Jovian and Saturnian satellites in accretion disks
Solar System Research, 2006The properties of gas-dust disks that surrounded Jupiter and Saturn during the final stage of their formation are analyzed. The sizes of the disks are determined by the total planetocentric angular momentum of the matter accreted by planets and correspond to the sizes of the orbits of their largest satellites.
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