I. Temperatures of polar ice deposits on Mercury and the Moon. II. Jovian atmospheric dynamics from Galileo imaging

Locations on Mercury that produce ice-like radar responses lie within impact craters that have very cold, permanently shaded floors. The retention of possible ice deposits is determined largely by their temperature. We present model-calculated temperatures of flat surfaces and surfaces within bowl-shaped and flat-floored polar impact craters. Our model includes appropriate insolation cycles, realistic crater shapes, multiple scattering of sunlight and infrared radiation, and depth and temperature-dependent regolith thermophysical properties. Meter-thick deposits of water ice are stable to evaporation over the age of the solar system if located in the permanently shaded portions of flat-floored craters within ;During the first six orbits of the Galileo spacecraft's prime mission, the Solid State Imaging system acquired multispectral image mosaics of Jupiter's Great Red Spot, an equatorial belt/zone boundary, a "5-...