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Planetary Formation: From the Earth and Moon to Extrasolar Giant PlanetsAn overview of current theories of star and planet formation is presented. These models are based upon observations of the Solar System and of young stars and their environments. They predict that rocky planets should form around most single stars, although it is possible that in some cases such planets are lost to orbital decay within the protoplanetary disk. The frequency of formation of gas giant planets is more difficult to predict theoretically. Terrestrial planets are believed to grow via pairwise accretion until the spacing of planetary orbits becomes large enough that the configuration is stable for the age of the system. Giant planets begin their growth like terrestrial planets, but they become massive enough that they are able to accumulate substantial amounts of gas before the protoplanetary disk dissipates. Specific issues to be discussed include: (1) how large a solid core is needed to initiate rapid accumulation of gas? (2) can giant planets form very close to stars? (3) could a giant impact leading to lunar formation have occurred approximately 100 million years after the condensation of the oldest meteorites?
Document ID
20020080688
Acquisition Source
Ames Research Center
Document Type
Conference Paper
Authors
Lissauer, Jack
(NASA Ames Research Center Moffett Field, CA United States)
DeVincenzi, Donald
Date Acquired
August 20, 2013
Publication Date
January 1, 1999
Subject Category
Astrophysics
Meeting Information
Meeting: Colloquium at NYU and 1st talk at Dark Matter in the Solar System Conference
Location: Paris
Country: France
Start Date: May 5, 1999
End Date: May 27, 1999
Funding Number(s)
PROJECT: RTOP 344-30-50-01
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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