The cratering event produced by the Deep Impact mission is a unique
experimental opportunity, beyond the capability of Earth-based laboratories
with regard to the impacting energy, target material, space environment,
and extremely low-gravity field. Consequently, impact cratering theory
and modeling play an important role in this mission, from initial
inception to final data analysis. Experimentally derived impact cratering
scaling laws provide us with our best estimates for the crater diameter,
depth, and formation time: critical in the mission planning stage
for producing the flight plan and instrument specifications. Cratering
theory has strongly influenced the impactor design, producing a probe
that should produce the largest possible crater on the surface of
Tempel 1 under a wide range of scenarios. Numerical hydrocode modeling
allows us to estimate the volume and thermodynamic characteristics
of the material vaporized in the early stages of the impact. Hydrocode
modeling will also aid us in understanding the observed crater excavation
process, especially in the area of impacts into porous materials.
Finally, experimentally derived ejecta scaling laws and modeling
provide us with a means to predict and analyze the observed behavior
of the material launched from the comet during crater excavation,
and may provide us with a unique means of estimating the magnitude
of the comet's gravity field and by extension the mass and density
of comet Tempel 1.
%0 Journal Article
%1 Richardson2005
%A Richardson, J. E.
%A Melosh, H. J.
%A Artemeiva, N. A.
%A Pierazzo, E.
%D 2005
%J Space Science Reviews
%K BREAKUP; CODE COMET DENSITY; HALLEY; SHOEMAKER-LEVY-9; SIZE; TARGET;
%N 1-2
%P 241--267
%T Impact cratering theory and modeling for the Deep Impact mission: From mission planning to data analysis
%V 117
%X The cratering event produced by the Deep Impact mission is a unique
experimental opportunity, beyond the capability of Earth-based laboratories
with regard to the impacting energy, target material, space environment,
and extremely low-gravity field. Consequently, impact cratering theory
and modeling play an important role in this mission, from initial
inception to final data analysis. Experimentally derived impact cratering
scaling laws provide us with our best estimates for the crater diameter,
depth, and formation time: critical in the mission planning stage
for producing the flight plan and instrument specifications. Cratering
theory has strongly influenced the impactor design, producing a probe
that should produce the largest possible crater on the surface of
Tempel 1 under a wide range of scenarios. Numerical hydrocode modeling
allows us to estimate the volume and thermodynamic characteristics
of the material vaporized in the early stages of the impact. Hydrocode
modeling will also aid us in understanding the observed crater excavation
process, especially in the area of impacts into porous materials.
Finally, experimentally derived ejecta scaling laws and modeling
provide us with a means to predict and analyze the observed behavior
of the material launched from the comet during crater excavation,
and may provide us with a unique means of estimating the magnitude
of the comet's gravity field and by extension the mass and density
of comet Tempel 1.
@article{Richardson2005,
abstract = {The cratering event produced by the Deep Impact mission is a unique
experimental opportunity, beyond the capability of Earth-based laboratories
with regard to the impacting energy, target material, space environment,
and extremely low-gravity field. Consequently, impact cratering theory
and modeling play an important role in this mission, from initial
inception to final data analysis. Experimentally derived impact cratering
scaling laws provide us with our best estimates for the crater diameter,
depth, and formation time: critical in the mission planning stage
for producing the flight plan and instrument specifications. Cratering
theory has strongly influenced the impactor design, producing a probe
that should produce the largest possible crater on the surface of
Tempel 1 under a wide range of scenarios. Numerical hydrocode modeling
allows us to estimate the volume and thermodynamic characteristics
of the material vaporized in the early stages of the impact. Hydrocode
modeling will also aid us in understanding the observed crater excavation
process, especially in the area of impacts into porous materials.
Finally, experimentally derived ejecta scaling laws and modeling
provide us with a means to predict and analyze the observed behavior
of the material launched from the comet during crater excavation,
and may provide us with a unique means of estimating the magnitude
of the comet's gravity field and by extension the mass and density
of comet Tempel 1.},
added-at = {2009-11-03T20:21:25.000+0100},
author = {Richardson, J. E. and Melosh, H. J. and Artemeiva, N. A. and Pierazzo, E.},
biburl = {https://www.bibsonomy.org/bibtex/29a3bb6b3ea69048dc9885b9e15c8d8b3/svance},
citedreferences = {ANDERSON CE, 1987, INT J IMPACT ENG, V5, P33 ; ANDERSON JLB, 2003, J GEOPHYS RES-PLANET, V108, P13 ; ARTEMIEVA NA, 2001, LUN PLAN I C ABST, V32, P1431 ; ASPHAUG E, 1994, Nature, V370, P120 ; BRANDT JC, 2004, INTRO COMETS ; BROWNLEE DE, 2004, Science, V304, P1764 ; CHAMBERLAIN JW, 1987, THEORY PLANETARY ATM ; CINTALA MJ, 1999, METEORIT PLANET SCI, V34, P605 ; COLLINS GS, 2004, METEORIT PLANET SCI, V39, P217 ; CROFT SK, 1981, MULTIRING BASINS, P207 ; GEISSLER P, 1996, Icarus, V120, P140 ; GRADY DE, 1987, FRACTURE MECH ROCK, P429 ; HEIKEN GH, 1991, LUNAR SOURCEBOOK ; HOLSAPPLE KA, 1980, LUNAR PLANET SCI, V11, P2379 ; HOLSAPPLE KA, 1982, J GEOPHYS RES, V87, P1849 ; HOUSEN KR, 1983, J GEOPHYS RES, V88, P2485 ; JESSBERGER EK, 1999, SPACE SCI REV, V90, P91 ; LARSON DB, 1977, UCRL52204 ; LISSE CM, 2004, IN PRESS Icarus ; LOVE SG, 1993, Icarus, V105, P216 ; MCGLAUN JM, 1990, INT J IMPACT ENG, V10, P351 ; MELOSH HJ, 1989, IMPACT CRATERING GEO ; MELOSH HJ, 1999, ANNU REV EARTH PL SC, V27, P385 ; MELOSH HJ, 2000, LUNAR PLANET SCI, V31, P1903 ; NOLAN MC, 1996, Icarus, V124, P359 ; NORDYKE MD, 1962, J GEOPHYS RES, V67, P1965 ; Peale SJ, 1989, Icarus, V82, P36 ; PIERAZZO E, 2001, ESF IMPACT 5 CATASTR ; POORMON KL, 1995, INT J IMPACT ENG 2, V17, P639 ; RUBIN MB, 2000, INT J SOLIDS STRUCT, V37, P1841 ; SAGDEEV RZ, 1988, Nature, V331, P240 ; SCHMIDT RM, 1987, INT J IMPACT ENG, V5, P543 ; SCHULTZ PH, 2002, LUN PLAN I C ABST, V33, P1875 ; SCOTTI JV, 1993, Nature, V365, P733 ; SHUVALOV VV, 1999, SHOCK WAVES, V9, P381 ; TAYLOR SR, 1982, PLANETARY SCI LUNAR ; THOMPSON SL, 1972, SCRR710714 ; WERNER RA, 1994, CELEST MECH DYN ASTR, V59, P253 ; WROTH CP, 1983, GEOTECHNIQUE, V33, P32 ; WUNNEMANN K, 2003, PLANET SPACE SCI, V51, P831},
interhash = {5f09f74bdc11fed826da769b9f820485},
intrahash = {9a3bb6b3ea69048dc9885b9e15c8d8b3},
journal = {Space Science Reviews},
keywords = {BREAKUP; CODE COMET DENSITY; HALLEY; SHOEMAKER-LEVY-9; SIZE; TARGET;},
number = {1-2},
owner = {svance},
pages = {241--267},
timestamp = {2009-11-03T20:22:11.000+0100},
title = {Impact cratering theory and modeling for the Deep Impact mission: From mission planning to data analysis},
volume = 117,
year = 2005
}