%0 Journal Article %1 McEwen2000 %A McEwen, A. S. %A Belton, M. J. S. %A Breneman, H. H. %A Fagents, S. A. %A Geissler, P. %A Greeley, R. %A Head, J. W. %A Hoppa, G. %A Jaeger, W. L. %A Johnson, T. V. %A Keszthelyi, L. %A Klaasen, K. P. %A Lopes-Gautier, R. %A Magee, K. P. %A Milazzo, M. P. %A Moore, J. M. %A Pappalardo, R. T. %A Phillips, C. B. %A Radebaugh, J. %A Schubert, G. %A Schuster, P. %A Simonelli, D. P. %A Sullivan, R. %A Thomas, P. C. %A Turtle, E. P. %A Williams, D. A. %D 2000 %J Science %K imported %N 5469 %P 1193--1198 %T Galileo at Io: Results from high-resolution imaging %V 288 %X During late 1999/early 2000, the solid state imaging experiment on the Galileo spacecraft returned more than 100 high-resolution (5 to 500 meters per pixel) images of volcanically active lo. We observed an active Lava lake, an active curtain of lava, active Lava flows, calderas, mountains, plateaus, and plains. Several of the sulfur dioxide-rich plumes are erupting from distal flows, rather than from the source of silicate Lava (caldera or fissure, often with red pyroclastic deposits). Most of the active flows in equatorial regions are being emplaced slowly beneath insulated crust, but rapidly emplaced channelized flows are also found at all latitudes. There is no evidence for high-viscosity Lava, but some bright flows may consist of sulfur rather than mafic silicates. The mountains, plateaus, and calderas are strongly influenced by tectonics and gravitational collapse. Sapping channels and scarps suggest that many portions of the upper similar to 1 kilometer are rich in volatiles.

@article{McEwen2000, abstract = {During late 1999/early 2000, the solid state imaging experiment on the Galileo spacecraft returned more than 100 high-resolution (5 to 500 meters per pixel) images of volcanically active lo. We observed an active Lava lake, an active curtain of lava, active Lava flows, calderas, mountains, plateaus, and plains. Several of the sulfur dioxide-rich plumes are erupting from distal flows, rather than from the source of silicate Lava (caldera or fissure, often with red pyroclastic deposits). Most of the active flows in equatorial regions are being emplaced slowly beneath insulated crust, but rapidly emplaced channelized flows are also found at all latitudes. There is no evidence for high-viscosity Lava, but some bright flows may consist of sulfur rather than mafic silicates. The mountains, plateaus, and calderas are strongly influenced by tectonics and gravitational collapse. Sapping channels and scarps suggest that many portions of the upper similar to 1 kilometer are rich in volatiles.}, added-at = {2009-11-03T20:21:25.000+0100}, author = {McEwen, A. S. and Belton, M. J. S. and Breneman, H. H. and Fagents, S. A. and Geissler, P. and Greeley, R. and Head, J. W. and Hoppa, G. and Jaeger, W. L. and Johnson, T. V. and Keszthelyi, L. and Klaasen, K. P. and Lopes-Gautier, R. and Magee, K. P. and Milazzo, M. P. and Moore, J. M. and Pappalardo, R. T. and Phillips, C. B. and Radebaugh, J. and Schubert, G. and Schuster, P. and Simonelli, D. P. and Sullivan, R. and Thomas, P. C. and Turtle, E. P. and Williams, D. A.}, biburl = {https://www.bibsonomy.org/bibtex/2f02b2547927cad916fc2450dcca3636f/svance}, citedreferences = {ACTON DS, UNPUB ; BRUNO BC, 1992, GEOPHYS RES LETT, V19, P305 ; CARR MH, 1998, Icarus, V135, P146 ; DAVIES AG, 1999, LUNAR PLANET SCI, V30 ; FAGENTS SA, 1999, EOS S, V80, F625 ; GEISSLER PE, 1999, Icarus, V140, P265 ; GEISSLER PE, 1999, Science, V285, P870 ; HEAD JW, 2000, LUNAR PLANET SCI, V31 ; HESLOP SE, 1989, B VOLCANOL, V51, P415 ; HON K, 1994, GEOL SOC AM BULL, V106, P251 ; JOHNSON TV, 1982, SATELLITES JUPITER, P634 ; KARGEL JS, 1999, Icarus, V142, P249 ; KESZTHELYI L, IN PRESS J GEOPHYS R ; KESZTHELYI L, 1997, GEOPHYS RES LETT, V24, P2463 ; KESZTHELYI L, 1997, Icarus, V130, P437 ; KIEFFER SW, 1982, SATELLITES JUPITER, P647 ; KIEFFER SW, 2000, Science, V288, P1204 ; LOPESGAUTIER R, 1999, Icarus, V140, P243 ; LOPESGAUTIER R, 2000, Science, V288, P1201 ; MATTOX TN, 1993, B VOLCANOL, V55, P407 ; MCCAULEY JF, 1979, Nature, V280, P736 ; MCEWEN AS, IN PRESS ENV EFFECTS ; MCEWEN AS, 1998, Icarus, V135, P181 ; MCEWEN AS, 1998, Science, V281, P87 ; MOORE JM, 2000, LUNAR PLANET SCI, V31 ; ONEIL WJ, 1997, FLIGHT PROJECT GALIL ; PHILLIPS CB, 2000, THESIS U ARIZONA TUC ; SCHENK PM, 1998, Science, V279, P1514 ; SELF S, 1997, LARGE IGNEOUS PROVIN, P381 ; SPENCER JR, 1997, GEOPHYS RES LETT, V24, P2471 ; SPENCER JR, 2000, Science, V288, P1198 ; SPENCER JR, 2000, Science, V288, P1208 ; STANSBERRY JA, 1997, GEOPHYS RES LETT, V24, P2455 ; THORAINSSON S, 1953, B VOLCANOL, V2, P1 ; WILLIAMS DA, IN PRESS EOS S ; WILLIAMS DA, 2000, J GEOPHYS RES-PLANET, V105, P1671 ; WILSON L, 1983, Nature, V302, P663}, interhash = {b4f594dd492b66784004053acdcb183e}, intrahash = {f02b2547927cad916fc2450dcca3636f}, journal = {Science}, keywords = {imported}, number = 5469, owner = {svance}, pages = {1193--1198}, timestamp = {2009-11-03T20:22:01.000+0100}, title = {Galileo at Io: Results from high-resolution imaging}, volume = 288, year = 2000 }