TY - JOUR
T1 - Collisional and dynamical history of Ida
AU - Greenberg, Richard
AU - Bottke, William F.
AU - Nolan, Michael
AU - Geissler, Paul
AU - Petit, Jean Marc
AU - Durda, Daniel D.
AU - Asphaug, Erik
AU - Head, James
N1 - Funding Information:
This work was made possible by Professor Greenberg’s participation on the Imaging Team of the NASA/JPL Galileo mission. We are grateful to the members of the Imaging Team, led by Dr. M. Belton, for comments and critiques on this specific work, and for providing a stimulating intellectual setting for the analysis of Galileo data. We thank all members of the Galileo project for their contributions to obtaining the magnificent imagery returned by the spacecraft. Careful reviews of the manuscript by Paolo Paolicchi and Eileen Ryan led to considerable improvements. Data processing for the work reported here was managed by Joe Plass-mann. Undergraduate assistant Terry Hurford helped with the analysis of orbital stability for Dactyl. Much of the analysis reported here was supported by a grant from NASA’s Planetary Geology and Geophysics program.
PY - 1996/3
Y1 - 1996/3
N2 - The history of Ida is constrained by its membership in the Koronis family, its satellite Dactyl, the record of impacts left on its surface, and other dynamical, morphological, and spectral properties. Models of crater production and comparably effective erasure processes, combined with the current size - frequency distribution of craters, suggest that the age of the surface is either about 50 myr or > 1 byr. The younger age may be inconsistent with the degraded appearance of many craters, while the older age conflicts with the collisional life expectancy of Dactyl. Consideration of Dactyl's evolution may resolve this issue as well as shed light on the formation of Dactyl, the density of Ida, and possible source regions for Ida and Dactyl within the Koronis parent body.
AB - The history of Ida is constrained by its membership in the Koronis family, its satellite Dactyl, the record of impacts left on its surface, and other dynamical, morphological, and spectral properties. Models of crater production and comparably effective erasure processes, combined with the current size - frequency distribution of craters, suggest that the age of the surface is either about 50 myr or > 1 byr. The younger age may be inconsistent with the degraded appearance of many craters, while the older age conflicts with the collisional life expectancy of Dactyl. Consideration of Dactyl's evolution may resolve this issue as well as shed light on the formation of Dactyl, the density of Ida, and possible source regions for Ida and Dactyl within the Koronis parent body.
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U2 - 10.1006/icar.1996.0040
DO - 10.1006/icar.1996.0040
M3 - Article
AN - SCOPUS:0030101401
SN - 0019-1035
VL - 120
SP - 106
EP - 118
JO - Icarus
JF - Icarus
IS - 1
ER -