%0 Journal Article %1 Turtle2001a %A Turtle, E. P. %A Pierazzo, E. %D 2001 %J Science %K CONSTRAINTS; EVIDENCE; FEATURES; GEOLOGICAL LIQUID MODEL; NONSYNCHRONOUS OCEAN; ROTATION; STATE SUBSURFACE WATER; %N 5545 %P 1326--1328 %T Thickness of a European ice shell from impact crater simulations %V 294 %X Several impact craters on Jupiter's satellite Europa exhibit central peaks. On the terrestrial planets, central peaks consist of fractured but competent rock uplifted during cratering. Therefore, the observation of central peaks on Europa indicates that an ice layer must be sufficiently thick that the impact events did not completely penetrate it. We conducted numerical simulations of vapor and melt production during cratering of water ice layers overlying liquid water to estimate the thickness of Europa's icy crust. Because impacts disrupt material well beyond the zone of partial melting, our simulations put a lower limit on ice thickness at the locations and times of impact. We conclude that the ice must be more than 3 to 4 kilometers thick.

@article{Turtle2001a, abstract = {Several impact craters on Jupiter's satellite Europa exhibit central peaks. On the terrestrial planets, central peaks consist of fractured but competent rock uplifted during cratering. Therefore, the observation of central peaks on Europa indicates that an ice layer must be sufficiently thick that the impact events did not completely penetrate it. We conducted numerical simulations of vapor and melt production during cratering of water ice layers overlying liquid water to estimate the thickness of Europa's icy crust. Because impacts disrupt material well beyond the zone of partial melting, our simulations put a lower limit on ice thickness at the locations and times of impact. We conclude that the ice must be more than 3 to 4 kilometers thick.}, added-at = {2009-11-03T20:21:25.000+0100}, author = {Turtle, E. P. and Pierazzo, E.}, biburl = {https://www.bibsonomy.org/bibtex/29c1bdd48cc6dccd4a9129fa2c16b75f2/svance}, citedreferences = {ANDERSON JD, 1998, Science, V281, P2019 ; ASPHAUG E, 1996, Icarus, V121, P225 ; BROOKSHAW L, 1998, WORKING PAPER SERIES ; CARR MH, 1998, Nature, V391, P363 ; Cassen PM, 1982, SATELLITES JUPITER, P93 ; DURHAM WB, 1997, J GEOPHYS RES-PLANET, V102, P16293 ; GEISSLER PE, 1998, Nature, V391, P368 ; GEISSLER PE, 2001, LUNAR PLANET SCI C, V32, P2068 ; Greenberg R, 2000, J GEOPHYS RES-PLANET, V105, P17551 ; GRIEVE RAF, 1981, P LUNAR PLANET SCI, V12, P37 ; HELFENSTEIN P, 1985, Icarus, V61, P175 ; HOPPA G, 1999, Icarus, V137, P341 ; HOPPA GV, 1999, Science, V285, P1899 ; KIVELSON MG, 2000, Science, V289, P1340 ; MCEWEN AS, 1986, Nature, V321, P49 ; MCKINNON WB, 1999, GEOPHYS RES LETT, V26, P951 ; MELOSH HJ, 1982, J GEOPHYS RES, V87, P371 ; MELOSH HJ, 1989, IMPACT CRATERING GEO ; MOORE JM, 1998, Icarus, V135, P127 ; MOORE JM, 2001, Icarus, V151, P93 ; OBRIEN DP, IN PRESS Icarus ; Ojakangas GW, 1989, Icarus, V81, P220 ; PAPPALARDO RT, 1998, Nature, V391, P365 ; PAPPALARDO RT, 1999, J GEOPHYS RES-PLANET, V104, P24015 ; PIETERS CM, 1982, Science, V215, P59 ; PROCKTER LM, 2000, Science, V289, P941 ; RATHBUN JA, 1998, GEOPHYS RES LETT, V25, P4157 ; ROSS MN, 1987, Nature, V325, P133 ; SCHENK PM, 1989, Icarus, V79, P75 ; SCHMIDT RM, 1987, INT J IMPACT ENG, V5, P543 ; Squyres SW, 1983, Nature, V301, P225 ; THOMPSON SL, 1972, SAND892951 ; THOMPSON SL, 1979, SAND771339 ; ZAHNLE K, 1998, Icarus, V136, P202 ; ZIMMER C, 2000, Icarus, V147, P329}, interhash = {426d3ae9d957fc404a8cafe25f05d602}, intrahash = {9c1bdd48cc6dccd4a9129fa2c16b75f2}, journal = {Science}, keywords = {CONSTRAINTS; EVIDENCE; FEATURES; GEOLOGICAL LIQUID MODEL; NONSYNCHRONOUS OCEAN; ROTATION; STATE SUBSURFACE WATER;}, number = 5545, owner = {svance}, pages = {1326--1328}, timestamp = {2009-11-03T20:22:19.000+0100}, title = {Thickness of a European ice shell from impact crater simulations}, volume = 294, year = 2001 }