Αποτελέσματα Αναζήτησης
1 Σεπ 2010 · Its main ring is located at 1.71R J ≤ r ≤ 1.81R J (the planet's radius R J ≃ 71,398 km) with an optical depth τ ≃ 10 −5. The main ring consists of ‘large bodies’ in the centimeter to meter size range [Showalter et al., 2007] and also a large population of small dust particles in the 0.1 ≤ a ≤ 100 μm size range. The small ...
Lorentz resonances. Electromagnetic forces have been shown to be significant for jovian ring particles, especially as the possible cause for out-of plane motion 10,12-15.
Compare and contrast the internal heat sources of the giant planets. Describe the discovery and characteristics of the giant planets’ magnetic fields. Let us now examine the four giant (or jovian) planets in more detail.
1 Ιαν 2012 · Due to the large charge-to-mass ratio, their dynamics is dominated by electromagnetic forces, which lead to the high-speed ejection from the planetary magnetospheres and the dust impact bursts reported from the in situ dust measurements (i.e., the dust stream phenomena).
Abstract. A comparison of the Jovian and Saturnian rings is made by reviewing the recent advances in planetary spacecraft exploration and theoretical study. Two main issues are ad-dressed, namely, the different structures of these two planetary ring systems and the water ice composition of the Saturnian rings.
Each of the Jovian planets has several characteristics in common. While Saturn’s bright rings are the most visible and well known, fainter and darker rings have . been seen around Jupiter, Uranus, and Neptune. The Jovian planets also are distinctive for having many moons.
1 Ιαν 2020 · Seasonal changes in Saturn’s atmosphere are thought to be caused by the rings, which cast shadows on the atmosphere and shield some of the planet from direct sunlight.
