Titlebook: Solar and Extra-Solar Planetary Systems; Lectures Held at the Iwan P. Williams,Nicolas Thomas Book 2001 Springer-Verlag Berlin Heidelberg 2

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The Giant Planets,the icy giants, Uranus and neptune, which are less massive and mostly made of ices. This chapter reviews their thermal structures, their chemical compositions, and their cloud structures. The abundance ratios of the giant planets, inferred from their spectral properties, are reviewed, and the implic

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Dynamics of the Solar System, the properties of the planetary disturbing function is presented showing how the dynamics of resonances can be understood using a pendulum approximation. Newtonian gravitation also permits chaotic motion. The properties of chaotic systems are examined together with applications to the long-term dyn

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Photometry of Resolved Planetary Surfaces,adiance into parameters which describe the surface properties can be confusing, however, because of differences in nomenclature and definition used by authors. Here, we present terms and definitions for some of the most commonly used quantities used in broad-band photometry leading to a brief descri

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Physical Processes Associated with Planetary Satellites, planetary physics. Here we discuss some of the physical processes affecting the shapes, surfaces and atmospheres of planetary satellites and illustrate them with examples from throughout the Solar System. In particular, satellite sphericity, cratering, resurfacing, the effects of surface frosts, th

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Light Scattering in the Martian Atmosphere: Effects on Surface Photometry,ve and increasing rapidly. Each individual aspect can only be addressed adequately in a relatively large review. Here, we concentrate on the atmosphere and in particular on the dust content. The dust influences our interpretation of remote sensing data in subtle ways which require extensive modellin

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Dust in the Solar System and in Other Planetary Systems,d by the collapse of a cloud of dust and gas. An accretion disk is formed around the central body and the planetary system eventually evolves. Some of the original dust particles are blown out-off the newly forming solar system by solar radiation and solar wind pressure,p ossibly being deflected in