%0 Journal Article %1 Keszthelyi2001 %A Keszthelyi, L. %A McEwen, A. S. %A Phillips, C. B. %A Milazzo, M. %A Geissler, P. %A Turtle, E. P. %A Radebaugh, J. %A Williams, D. A. %A Simonelli, D. P. %A Breneman, H. H. %A Klaasen, K. P. %A Levanas, G. %A Denk, T. %D 2001 %J Journal of Geophysical Research-Planets %K EMISSION; ERUPTIONS; FLOW-FIELD; HOT-SPOTS; INFRARED KILAUEA LAVA MAPPING MODELS; PLUME SILICATE SPECTROMETER; TEMPERATURE; THERMAL VOLCANISM; VOLCANO; %N E12 %P 33025--33052 %T Imaging of volcanic activity on Jupiter's moon Io by Galileo during the Galileo Europa Mission and the Galileo Millennium Mission. %V 106 %X The Solid-State Imaging (SSI) instrument provided the first high- and medium-resolution views of Io as the Galileo spacecraft closed in on the volcanic body in late 1999 and early 2000. While each volcanic center has many unique features, the majority can be placed into one of two broad categories. The "Promethean" eruptions, typified by the volcanic center Prometheus, are characterized by long-lived steady eruptions producing a compound flow field emplaced in an insulating manner over a period of years to decades. In contrast, "Pillanian" eruptions are characterized by large pyroclastic deposits and short-lived but high effusion rate eruptions from fissures feeding open-channel or open-sheet flows. Both types of eruptions commonly have similar to100-km-tall, bright, SO2-rich plumes forming near the flow fronts and smaller deposits of red material that mark the vent for the silicate lavas.

@article{Keszthelyi2001, abstract = {The Solid-State Imaging (SSI) instrument provided the first high- and medium-resolution views of Io as the Galileo spacecraft closed in on the volcanic body in late 1999 and early 2000. While each volcanic center has many unique features, the majority can be placed into one of two broad categories. The "Promethean" eruptions, typified by the volcanic center Prometheus, are characterized by long-lived steady eruptions producing a compound flow field emplaced in an insulating manner over a period of years to decades. In contrast, "Pillanian" eruptions are characterized by large pyroclastic deposits and short-lived but high effusion rate eruptions from fissures feeding open-channel or open-sheet flows. Both types of eruptions commonly have similar to100-km-tall, bright, SO2-rich plumes forming near the flow fronts and smaller deposits of red material that mark the vent for the silicate lavas.}, added-at = {2009-11-03T20:21:25.000+0100}, author = {Keszthelyi, L. and McEwen, A. S. and Phillips, C. B. and Milazzo, M. and Geissler, P. and Turtle, E. P. and Radebaugh, J. and Williams, D. A. and Simonelli, D. P. and Breneman, H. H. and Klaasen, K. P. and Levanas, G. and Denk, T.}, biburl = {https://www.bibsonomy.org/bibtex/2aaa4302b56e547e5ed5fc2000049fb5c/svance}, citedreferences = {BLANEY DL, 1995, Icarus, V113, P220 ; CARR MH, 1983, Icarus, V56, P476 ; CARR MH, 1986, J GEOPHYS RES-SOLID, V91, P3521 ; CLOW GD, 1980, Icarus, V44, P729 ; DAVIES AG, 1996, Icarus, V124, P45 ; DAVIES AG, 1997, GEOPHYS RES LETT, V24, P2447 ; DAVIES AG, 2000, Icarus, V148, P211 ; EATON JP, 1987, US GEOL SURV PROF PA, V1350, P1307 ; FISCHER HJ, 1990, Icarus, V83, P39 ; GEISSLER PE, 1999, Icarus, V140, P265 ; GEISSLER PE, 1999, Science, V285, P870 ; GOGUEN JD, 1988, Icarus, V76, P465 ; JAEGER W, 2001, LUNAR PLANET SCI C, V32, P2045 ; JOHNSON TV, 1988, Science, V242, P1280 ; KARGEL JS, 1999, Icarus, V142, P249 ; KAUAHIKAUA J, 1998, J GEOPHYS RES-SOL EA, V103, P27303 ; KESZTHELYI L, 1995, J GEOPHYS RES-SOLID, V100, P20411 ; KESZTHELYI L, 1997, GEOPHYS RES LETT, V24, P2463 ; KESZTHELYI L, 1998, J GEOPHYS RES-SOL EA, V103, P27447 ; KESZTHELYI L, 2000, J GEOPHYS RES-PLANET, V105, P15027 ; KESZTHELYI L, 2001, LUNAR PLANET SCI C, V32, P1523 ; KESZTHELYI LP, 1993, J VOLCANOL GEOTH RES, V59, P59 ; KIEFFER SW, 2000, Science, V288, P1204 ; KLAASEN KP, 1997, OPT ENG, V36, P3001 ; LOPESGAUTIER R, 1997, GEOPHYS RES LETT, V24, P2439 ; LOPESGAUTIER R, 1999, Icarus, V140, P243 ; LOPESGAUTIER R, 2000, Science, V288, P1201 ; LUNINE JI, 1985, Icarus, V64, P345 ; MATTOX TN, 1993, B VOLCANOL, V55, P407 ; MCEWEN AS, 1983, Icarus, V55, P191 ; MCEWEN AS, 1989, NASA SP, V494, P11 ; 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 ; MOORE HJ, 1987, 1350 US GEOL SURV, P1569 ; Ojakangas GW, 1986, Icarus, V66, P341 ; Peale SJ, 1979, Science, V203, P892 ; PEARL JC, 1982, SATELLITES JUPITER, P724 ; PHILLIPS CB, 2000, THESIS U ARIZONA TUC ; SARTORETTI P, 1995, J GEOPHYS RES-PLANET, V100, P7523 ; SCHABER GG, 1982, SATELLITES JUPITER, P556 ; Schubert G, 1981, Icarus, V47, P46 ; SELF S, 1997, GEOPH MONOG SERIES, V100, P381 ; SMITH BA, 1979, Nature, V280, P738 ; SMITH BA, 1979, Science, V204, P951 ; SPENCER JR, 1996, ANNU REV EARTH PL SC, V24, P125 ; SPENCER JR, 1997, GEOPHYS RES LETT, V24, P2451 ; SPENCER JR, 2000, Science, V288, P1198 ; SPENCER JR, 2000, Science, V288, P1208 ; STANSBERRY JA, 1997, GEOPHYS RES LETT, V24, P2455 ; STROM RG, 1981, J GEOPHYS RES, V86, P8593 ; THORDARSON T, 1993, B VOLCANOL, V55, P233 ; THORDARSON T, 1998, J GEOPHYS RES-SOL EA, V103, P27411 ; VEEDER GJ, 1994, J GEOPHYS RES, V99, P17095 ; WILLIAMS DA, 2000, J GEOPHYS RES-PLANET, V105, P1671 ; WILLIAMS DA, 2001, LUNAR PLANET SCI C, V32, P1220 ; WITTEBORN FC, 1979, Science, V203, P643 ; ZOLOTOV MY, 1999, Icarus, V141, P40 ; ZOLOTOV MY, 2000, GEOPHYS RES LETT, V27, P2789}, interhash = {d59d49f9b81a82365fe7b90b4ac5c4fc}, intrahash = {aaa4302b56e547e5ed5fc2000049fb5c}, journal = {Journal of Geophysical Research-Planets}, keywords = {EMISSION; ERUPTIONS; FLOW-FIELD; HOT-SPOTS; INFRARED KILAUEA LAVA MAPPING MODELS; PLUME SILICATE SPECTROMETER; TEMPERATURE; THERMAL VOLCANISM; VOLCANO;}, number = {E12}, owner = {svance}, pages = {33025--33052}, timestamp = {2009-11-03T20:21:54.000+0100}, title = {Imaging of volcanic activity on Jupiter's moon Io by Galileo during the Galileo Europa Mission and the Galileo Millennium Mission.}, volume = 106, year = 2001 }