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Planet formationModels of planetary formation are developed using the present single example of a planetary system, supplemented by limited astrophysical observations of star-forming regions and circumstellar disks. The solar nebula theory and the planetesimal hypothesis are discussed. The latter is found to provide a viable theory of the growth of the terrestrial planets, the cores of the giant planets, and the smaller bodies present in the solar system. The formation of solid bodies of planetary size should be a common event, at least around young stars which do not have binary companions orbiting at planetary distances. Stochastic impacts of large bodies provide sufficient angular momentum to produce the obliquities of the planets. The masses and bulk compositions of the planets can be understood in a gross sense as resulting from planetary growth within a disk whose temperature and surface density decreased with distance from the growing sun.
Document ID
19940036075
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Lissauer, Jack J.
(New York State Univ. Stony Brook; California Univ., Santa Barbara, United States)
Date Acquired
August 16, 2013
Publication Date
January 1, 1993
Publication Information
Publication: In: Annual review of astronomy and astrophysics. Vol. 31 (A94-12726 02-90)
Publisher: Annual Reviews, Inc.
Subject Category
Lunar And Planetary Exploration
Accession Number
94A12730
Funding Number(s)
CONTRACT_GRANT: NAGW-2837
CONTRACT_GRANT: NAGW-1107
CONTRACT_GRANT: NSF PHY-89-04035
Distribution Limits
Public
Copyright
Other

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