Download Encyclopedia of the Solar System ~ 1st Edition by Paul Weissman, Lucy-Ann McFadden, Torrence Johnson PDF

By Paul Weissman, Lucy-Ann McFadden, Torrence Johnson

The Encyclopedia of the sun approach offers a chain of entire and authoritative articles written by means of greater than 50 eminent planetary and area scientists. every one bankruptcy is self-contained but associated through cross-references to different comparable chapters. This superbly designed ebook is a needs to for the library astronomers and beginner star-gazers alike, actually for someone who needs to appreciate the character of our sun method. * Cross-referenced all through for simple comprehension* beautifully illustrated with over seven-hundred images, drawings, and diagrams, together with 36 colour plates* offers forty thematically prepared chapters by means of greater than 50 eminent individuals* handy glossaries of technical phrases introduce each one bankruptcy* Foreword written by way of astronaut Sally experience* particular site for the Encyclopedia at comprises author-recommended internet assets for more information, photos, and examine advancements relating to each one bankruptcy of this quantity

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Extra info for Encyclopedia of the Solar System ~ 1st Edition

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The clearing of the planetary zones has several interesting consequences. The dynamical interaction between the planets and the remaining planetesimals results in an exchange of angular momentum. Computer-based dynamical simulations have shown that this causes the semimajor axes of the planets to migrate radially. In general, Saturn, Uranus, and Neptune are expected to first move inward and then later outward as the ejection of material progresses. Jupiter, which ejects the most material because of its huge mass, migrates inward, but only by a few tenths of an astronomical unit.

At larger distances where the nebula was cooler, organic and icy THE SOLAR SYSTEM AND ITS PLACE IN THE GALAXY 27 FIGURE 12 Artist’s concept of the accretion disk in the solar nebula, showing the orbiting planetesimals and the proto-Sun at the center. ) grains would condense and these would combine with the silicates to form the cores of the giant planets. Because the total mass of ice and organics may have been several times the mass of silicates, the cores of the giant planets may actually have grown faster than the terrestrial planets interior to them.

As the dust grains fall inward, they experience a pressure from the increasing density of gas toward the center of the nebula. This slows and even halts the inward radial component of their motion. However, the dust grains can still move vertically with respect to the central plane of the nebula, as defined by the rotational angular momentum vector of the orginal cloud core. As a result, the grains settle toward the central plane. As the grains settle, they begin to collide with one another. The grains stick and quickly grow from microscopic to macroscopic objects, perhaps meters in size (initial agglomerations of grains may look very much like the suspected cometary IDP in Fig.

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