NASA Logo

NTRS

NTRS - NASA Technical Reports Server

Back to Results
Growth of planets from planetesimalsThe formation of terrestrial planets and the cores of Jovian planets is reviewed in the framework of the planetesimal hypothesis, wherein planets are assumed to grow via the pairwise accumulation of small solid bodies. The rate of (proto)planetary growth is determined by the size and mass of the protoplanet, the surface density of planetesimals, and the distribution of planetesimal velocities relative to the protoplanet. Planetesimal velocities are modified by mutual gravitational interactions and collisions, which convert energy present in the ordered relative motions of orbiting particles (Keplerian shear) into random motions and tend to reduce the velocities of the largest bodies in the swarm relative to those of smaller bodies, as well as by gas drag, which damps eccentricities and inclinations.
Document ID
19920001681
Acquisition Source
Legacy CDMS
Document Type
Other
Authors
Lissauer, Jack J.
(State Univ. of New York Stony Brook, NY, United States)
Stewart, Glen R.
(Colorado Univ. Boulder., United States)
Date Acquired
September 6, 2013
Publication Date
June 1, 1991
Publication Information
Publication: NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1990
Subject Category
Lunar And Planetary Exploration
Accession Number
92N10899
Funding Number(s)
CONTRACT_GRANT: NAGW-769
CONTRACT_GRANT: NAGW-1107
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

Available Downloads

There are no available downloads for this record.
No Preview Available