%0 Journal Article %1 Turtle2001 %A Turtle, E. P. %A Jaeger, W. L. %A Keszthelyi, L. P. %A McEwen, A. S. %A Milazzo, M. %A Moore, J. %A Phillips, C. B. %A Radebaugh, J. %A Simonelli, D. %A Chuang, F. %A Schuster, P. %D 2001 %J Journal of Geophysical Research-Planets %K ACTIVE HEAT; LITHOSPHERE; LO ORIGIN; SYSTEM; TOPOGRAPHY; VOLCANISM; %N E12 %P 33175--33199 %T Mountains on Io: High-resolution Galileo observations, initial interpretations, and formation models %V 106 %X During three close flybys in late 1999 and early 2000 the Galileo spacecraft acquired new observations of the mountains that tower above to's surface. These images have revealed surprising variety in the mountains' morphologies. They range from jagged peaks several kilometers high to lower, rounded structures. Some are very smooth, others are covered by numerous parallel ridges. Many mountains have margins that are collapsing outward in large landslides or series of slump blocks, but a few have steep, scalloped scarps. From these observations we can gain insight into the structure and material properties of to's crust as well as into the erosional processes acting on to. We have also investigated formation mechanisms proposed for these structures using finite-element analysis. Mountain formation might be initiated by global compression due to the high rate of global subsidence associated with to's high resurfacing rate; however, our models demonstrate that this hypothesis lacks a mechanism for isolating the mountains. The large fraction (similar to40%) of mountains that are associated with paterae suggests that in some cases these features are tectonically related. Therefore we have also simulated the stresses induced in to's crust by a combination of a thermal upwelling in the mantle with global lithospheric compression and have shown that this can focus compressional stresses. If this mechanism is responsible for some of Io's mountains, it could also explain the common association of mountains with paterae.

@article{Turtle2001, abstract = {During three close flybys in late 1999 and early 2000 the Galileo spacecraft acquired new observations of the mountains that tower above to's surface. These images have revealed surprising variety in the mountains' morphologies. They range from jagged peaks several kilometers high to lower, rounded structures. Some are very smooth, others are covered by numerous parallel ridges. Many mountains have margins that are collapsing outward in large landslides or series of slump blocks, but a few have steep, scalloped scarps. From these observations we can gain insight into the structure and material properties of to's crust as well as into the erosional processes acting on to. We have also investigated formation mechanisms proposed for these structures using finite-element analysis. Mountain formation might be initiated by global compression due to the high rate of global subsidence associated with to's high resurfacing rate; however, our models demonstrate that this hypothesis lacks a mechanism for isolating the mountains. The large fraction (similar to40%) of mountains that are associated with paterae suggests that in some cases these features are tectonically related. Therefore we have also simulated the stresses induced in to's crust by a combination of a thermal upwelling in the mantle with global lithospheric compression and have shown that this can focus compressional stresses. If this mechanism is responsible for some of Io's mountains, it could also explain the common association of mountains with paterae.}, added-at = {2009-11-03T20:21:25.000+0100}, author = {Turtle, E. P. and Jaeger, W. L. and Keszthelyi, L. P. and McEwen, A. S. and Milazzo, M. and Moore, J. and Phillips, C. B. and Radebaugh, J. and Simonelli, D. and Chuang, F. and Schuster, P.}, biburl = {https://www.bibsonomy.org/bibtex/2f867c46050a2a8c21a538f71ad3a4161/svance}, citedreferences = {BLANEY DL, 1995, Icarus, V113, P220 ; CARR MH, 1998, Icarus, V135, P146 ; CLOW GD, 1980, Icarus, V44, P729 ; FREED AM, 2001, J GEOPHYS RES-PLANET, V106, P20603 ; GEISSLER PE, 1999, Icarus, V140, P265 ; HEATH MJ, 1985, HEAT DETACHMENT CRUS, P50 ; JOHNSON TV, 1979, Nature, V280, P746 ; KESZTHELYI L, 1999, Icarus, V141, P415 ; KLAASEN KP, 1999, OPT ENG, V38, P1178 ; LOPESGAUTIER R, 1999, Icarus, V140, P243 ; MASURSKY H, 1979, Nature, V280, P725 ; MCCAULEY JF, 1979, Nature, V280, P736 ; MCEWEN AS, 1985, HEAT DETACHMENT CRUS, P76 ; MCEWEN AS, 1998, Icarus, V135, P181 ; MCEWEN AS, 2000, Science, V288, P1193 ; MCKINNON WB, 2001, Geology, V29, P103 ; MELOSH HJ, 1980, GEOPHYS J ROY ASTRON, V60, P333 ; NASH DB, 1986, SATELLITES, P629 ; OREILLY TC, 1981, GEOPHYS RES LETT, V8, P313 ; PHILLIPS CB, 2000, THESIS U ARIZ TUCSON ; SCHABER GG, 1980, Icarus, V43, P302 ; SCHABER GG, 1982, SATELLITES JUPITER, P556 ; SCHENK P, 1998, B AM ASTRON SOC, V30, P1121 ; SCHENK PM, 1998, Science, V279, P1514 ; SCHUSTER P, 2000, LUN PLAN SCI C, V31 ; SMITH BA, 1979, Science, V204, P951 ; SPENCER JR, 1997, GEOPHYS RES LETT, V24, P2451 ; TACKLEY PJ, 1999, EOS T AGU S, V80, F620 ; TACKLEY PJ, 2001, Icarus, V149, P79 ; Turcotte DL, 1982, GOEDYNAMICS APPL CON ; TURTLE EP, 1999, LUN PLAN SCI C, V30 ; TURTLE EP, 2000, LUN PLAN SCI C, V31 ; VEEDER GJ, 1994, J GEOPHYS RES, V99, P17095 ; WEBB EK, 1987, Icarus, V70, P348 ; WHITFORDSTARK JL, 1982, LUN PLAN SCI C, V13, P859}, interhash = {e6b63e4005c1191f14032ecab0f782d2}, intrahash = {f867c46050a2a8c21a538f71ad3a4161}, journal = {Journal of Geophysical Research-Planets}, keywords = {ACTIVE HEAT; LITHOSPHERE; LO ORIGIN; SYSTEM; TOPOGRAPHY; VOLCANISM;}, number = {E12}, owner = {svance}, pages = {33175--33199}, timestamp = {2009-11-03T20:22:19.000+0100}, title = {Mountains on Io: High-resolution Galileo observations, initial interpretations, and formation models}, volume = 106, year = 2001 }