A model for wind-extension of the Copernicus ejecta blanketThe interaction between crater ejecta and the transient wind from impact-shock vaporization is discussed. Based partly on Shoemaker's (1962) ballistic model of the Copernicus ejecta and partly on Rehfuss' (1972) treatment of lunar winds, a simple model is developed which indicates that if Copernicus were formed by a basaltic meteorite impacting at 20 km/s, then 3% of the ejecta mass would be sent beyond the maximum range expected from purely ballistic trajectories. That 3% mass would, however, shift the position of the outer edge of the ejecta blanket more than 400% beyond the edge of the ballistic blanket. For planetary bodies lacking an intrinsic atmosphere, the present model indicates that this form of hyperballistic transport can be very significant for small (no more than about 1 kg) ejecta fragments.
Document ID
19780060171
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Rehfuss, D. E. (San Diego State Univ. San Diego, CA, United States)
Michael, D. (San Diego State Univ. San Diego, CA, United States)
Anselmo, J. C. (San Diego State Univ. San Diego, CA, United States)
Kincheloe, N. K. (San Diego State University San Diego, Calif., United States)
Date Acquired
August 9, 2013
Publication Date
January 1, 1977
Subject Category
Lunar And Planetary Exploration
Meeting Information
Meeting: Symposium on Planetary Cratering Mechanics