%0 Journal Article %1 Radebaugh2001 %A Radebaugh, J. %A Keszthelyi, L. P. %A McEwen, A. S. %A Turtle, E. P. %A Jaeger, W. %A Milazzo, M. %D 2001 %J Journal of Geophysical Research-Planets %K ACTIVE ASH-FLOW CALDERAS; DIFFERENTIATION; DISTRIBUTION; EARTH FEATURES; GALILEO; GLOBAL INTERNAL STRUCTURE; TOPOGRAPHY; VENUS; VOLCANISM; %N E12 %P 33005--33020 %T Paterae on Io: A new type of volcanic caldera? %V 106 %X Paterae, defined by the International Astronomical Union as "irregular craters, or complex ones with scalloped edges," are some of the most prominent topographic features on Io. Paterae on Io are unique, yet in some aspects they resemble calderas known and studied on Earth, Mars, and Venus. They have steep walls, flat floors, and arcuate margins and sometimes exhibit nesting, all typical of terrestrial and Martian basalt shield calderas. However, they are much larger, many are irregular in shape, and they typically lack shields. Their great sizes (some >200 km diameter) and lack of associated volcanic edifices beg comparison with terrestrial ash flow calderas; however, there is no convincing evidence on Io for the high-silica erupted products or dome resurgence associated with this type of caldera. Ionian paterae seem to be linked with the eruption of large amounts of mafic to ultramafic lavas and colorful sulfur-rich materials that cover the floors and sometimes flow great distances away from patera margins. They are often angular in shape or area found adjacent to mountains or plateaus, indicating tectonic influences on their formation. A database of 417 paterae on Io measured from images with >3.2 km pixel (-1) resolution (80% of its surface) reveals that their mean diameter of 41.0 km is close to that for calderas of Mars (47.7 km), is smaller than that for Venus (similar to68 km), but dwarfs those for terrestrial basalt shield calderas (6.6 km) and ash flow calderas (18.7 km). Thirteen percent of all paterae are found adjacent to mountains, 42% have straight or irregular margins, and 8% are found atop low shields. Abundant, smaller paterae with more continuously active lava eruptions are found between 25degreesS and 25degreesN latitude, whereas fewer and larger paterae are found poleward of these latitudes. Patera distribution shows peaks at 330degreesW and 150degreesW longitude, likely related to the direction of greatest tidal massaging by Jupiter. Ionian patera formation may be explained by portions or combinations of models considered for formation of terrestrial calderas, yet their unusual characteristics may require new models with a greater role for tectonic processes.

@article{Radebaugh2001, abstract = {Paterae, defined by the International Astronomical Union as "irregular crater[s], or complex one[s] with scalloped edges," are some of the most prominent topographic features on Io. Paterae on Io are unique, yet in some aspects they resemble calderas known and studied on Earth, Mars, and Venus. They have steep walls, flat floors, and arcuate margins and sometimes exhibit nesting, all typical of terrestrial and Martian basalt shield calderas. However, they are much larger, many are irregular in shape, and they typically lack shields. Their great sizes (some >200 km diameter) and lack of associated volcanic edifices beg comparison with terrestrial ash flow calderas; however, there is no convincing evidence on Io for the high-silica erupted products or dome resurgence associated with this type of caldera. Ionian paterae seem to be linked with the eruption of large amounts of mafic to ultramafic lavas and colorful sulfur-rich materials that cover the floors and sometimes flow great distances away from patera margins. They are often angular in shape or area found adjacent to mountains or plateaus, indicating tectonic influences on their formation. A database of 417 paterae on Io measured from images with >3.2 km pixel (-1) resolution (80% of its surface) reveals that their mean diameter of 41.0 km is close to that for calderas of Mars (47.7 km), is smaller than that for Venus (similar to68 km), but dwarfs those for terrestrial basalt shield calderas (6.6 km) and ash flow calderas (18.7 km). Thirteen percent of all paterae are found adjacent to mountains, 42% have straight or irregular margins, and 8% are found atop low shields. Abundant, smaller paterae with more continuously active lava eruptions are found between 25degreesS and 25degreesN latitude, whereas fewer and larger paterae are found poleward of these latitudes. Patera distribution shows peaks at 330degreesW and 150degreesW longitude, likely related to the direction of greatest tidal massaging by Jupiter. Ionian patera formation may be explained by portions or combinations of models considered for formation of terrestrial calderas, yet their unusual characteristics may require new models with a greater role for tectonic processes.}, added-at = {2009-11-03T20:21:25.000+0100}, author = {Radebaugh, J. and Keszthelyi, L. P. and McEwen, A. S. and Turtle, E. P. and Jaeger, W. and Milazzo, M.}, biburl = {https://www.bibsonomy.org/bibtex/2fc399446942a2c9eaac302c1834ed267/svance}, citedreferences = {BEST MG, 1982, IGNEOUS METAMORPHIC ; BEST MG, 1989, GEOL SOC AM BULL, V101, P1076 ; BRIDGES NT, 1995, GEOPHYS RES LETT, V22, P2781 ; CARR MH, 1979, Nature, V280, P729 ; CARR MH, 1984, TM86246 NASA, P11 ; CRUMPLER LS, 1996, GEOL SOC SPEC PUBL, V110, P307 ; FRANCIS PW, 1993, VOLCANOES PLANETARY ; GASKELL RW, 1988, GEOPHYS RES LETT, V15, P581 ; GEISSLER PE, 1999, Icarus, V140, P265 ; Greenberg R, 1984, Icarus, V58, P186 ; HEAD JW, 1992, J GEOPHYS RES-PLANET, V97, P13153 ; JACKSON JA, 1997, GLOSSARY Geology ; JAEGER W, 2001, LUNAR PLANET SCI C, V32, P2045 ; JOHNSON TV, 1982, SATELLITES JUPITER, P634 ; KARAS GN, 1994, MAUNA LOA COMPILED V ; KARGEL JS, 1999, Icarus, V142, P249 ; KESZTHELYI L, 1997, Icarus, V130, P437 ; KESZTHELYI L, 1999, Icarus, V141, P415 ; LIPMAN PW, 1984, J GEOPHYS RES, V89, P8801 ; LIPMAN PW, 1997, B VOLCANOL, V59, P198 ; LOPESGAUTIER R, 1999, Icarus, V140, P243 ; LOPESGAUTIER R, 2000, Science, V288, P1201 ; MARSH BD, 1991, GEOL RUNDSCH, V80, P481 ; MCEWEN AS, 1985, J GEOPHYS RES, V90, P12345 ; MCEWEN AS, 1997, GEOPHYS RES LETT, V24, P2443 ; MCEWEN AS, 1998, Icarus, V135, P181 ; MCEWEN AS, 1998, Science, V281, P87 ; MCEWEN AS, 2000, Science, V288, P1193 ; MILAZZO MP, 2001, LUNAR PLANET SCI C, V32, P2089 ; MOORE JM, 1986, Icarus, V67, P181 ; PHILLIPS CB, 2000, THESIS U ARIZ TUCS ; PIKE RJ, 1981, 811038 US GEOL SURV ; RADEBAUGH J, 1999, THESIS BRIGHAM YOUNG ; ROSS MN, 1990, Icarus, V85, P309 ; SCHABER GG, 1982, SATELLITES JUPITER, P556 ; SMITH RL, 1968, GEOL SOC AM MEM, V116, P83 ; SMITH RL, 1979, GEOL SOC AM SPEC PAP, V180, P343 ; SPENCER JR, 2000, Science, V288, P1208 ; SPERA FJ, 1981, J VOLCANOL GEOTHERM, V11, P169 ; TACKLEY PJ, 2001, Icarus, V149, P79 ; WALKER GPL, 1988, J GEOPHYS RES-SOLID, V93, P14773 ; WILLIAMS H, 1941, U CALIF PUBLS GEOL S, V25, P239 ; WILSON L, 1983, Nature, V302, P663 ; WOOD CA, 1984, J GEOPHYS RES, V89, P8391}, interhash = {7ff3bd12af3c09e7e66848ada85f42c3}, intrahash = {fc399446942a2c9eaac302c1834ed267}, journal = {Journal of Geophysical Research-Planets}, keywords = {ACTIVE ASH-FLOW CALDERAS; DIFFERENTIATION; DISTRIBUTION; EARTH FEATURES; GALILEO; GLOBAL INTERNAL STRUCTURE; TOPOGRAPHY; VENUS; VOLCANISM;}, number = {E12}, owner = {svance}, pages = {33005--33020}, timestamp = {2009-11-03T20:22:11.000+0100}, title = {Paterae on Io: A new type of volcanic caldera?}, volume = 106, year = 2001 }