We present the observations of to acquired by the Solid State Imaging
(SSI) experiment during the Galileo Millennium Mission (GMM) and
the strategy we used to plan the exploration of to. Despite Galileo's
tight restrictions on data volume and downlink capability and several
spacecraft and camera anomalies due to the intense radiation. close
to Jupiter, there were many successful SSI observations during GMM.
Four giant, high-latitude plumes, including the largest plume ever
observed on to, were documented over a period of eight months; only
faint evidence of such plumes had been seen since the Voyager 2 encounter,
despite monitoring by Galileo during the previous five years. Moreover,
the source of one of the plumes was Tvashtar Catena, demonstrating
that a single site can exhibit remarkably diverse eruption styles-from
a curtain of lava fountains, to extensive surface flows, and finally
a similar to 400 km high plume-over a relatively short period of
time (similar to 13 months between orbits 125 and G29). Despite this
substantial activity, no evidence of any truly new volcanic center
was seen during the six years of Galileo observations. The recent
observations also revealed details of mass wasting processes acting
on to. Slumping and landsliding dominate and occur in close proximity
to each other, demonstrating spatial variation in material properties
over distances of several kilometers. However, despite the ubiquitous
evidence for mass wasting, the rate of volcanic resurfacing seems
to dominate; the floors of paterae in proximity to mountains are
generally free of debris. Finally, the highest resolution observations
obtained during Galileo's final encounters with to provided further
evidence for a wide diversity of surface processes at work on to.
(C) 2003 Elsevier Inc. All rights reserved.
%0 Journal Article
%1 Turtle2004
%A Turtle, E. P.
%A Keszthelyi, L. P.
%A McEwen, A. S.
%A Radebaugh, J.
%A Milazzo, M.
%A Simonelli, D. P.
%A Geissler, P.
%A Williams, D. A.
%A Perry, J.
%A Jaeger, W. L.
%A Klaasen, K. P.
%A Breneman, H. H.
%A Denk, T.
%A Phillips, C. B.
%D 2004
%J Icarus
%K ACTIVE CALIBRATION; EMPLACEMENT; ERUPTION; FLOW FLOWS; IO; JUPITERS MISSION; MOON MOUNTAINS; PLUMES SULFUR SYSTEM; VOLCANISM;
%N 1
%P 3--28
%T The final Galileo SSI observations of Io: orbits G28-I33
%V 169
%X We present the observations of to acquired by the Solid State Imaging
(SSI) experiment during the Galileo Millennium Mission (GMM) and
the strategy we used to plan the exploration of to. Despite Galileo's
tight restrictions on data volume and downlink capability and several
spacecraft and camera anomalies due to the intense radiation. close
to Jupiter, there were many successful SSI observations during GMM.
Four giant, high-latitude plumes, including the largest plume ever
observed on to, were documented over a period of eight months; only
faint evidence of such plumes had been seen since the Voyager 2 encounter,
despite monitoring by Galileo during the previous five years. Moreover,
the source of one of the plumes was Tvashtar Catena, demonstrating
that a single site can exhibit remarkably diverse eruption styles-from
a curtain of lava fountains, to extensive surface flows, and finally
a similar to 400 km high plume-over a relatively short period of
time (similar to 13 months between orbits 125 and G29). Despite this
substantial activity, no evidence of any truly new volcanic center
was seen during the six years of Galileo observations. The recent
observations also revealed details of mass wasting processes acting
on to. Slumping and landsliding dominate and occur in close proximity
to each other, demonstrating spatial variation in material properties
over distances of several kilometers. However, despite the ubiquitous
evidence for mass wasting, the rate of volcanic resurfacing seems
to dominate; the floors of paterae in proximity to mountains are
generally free of debris. Finally, the highest resolution observations
obtained during Galileo's final encounters with to provided further
evidence for a wide diversity of surface processes at work on to.
(C) 2003 Elsevier Inc. All rights reserved.
@article{Turtle2004,
abstract = {We present the observations of to acquired by the Solid State Imaging
(SSI) experiment during the Galileo Millennium Mission (GMM) and
the strategy we used to plan the exploration of to. Despite Galileo's
tight restrictions on data volume and downlink capability and several
spacecraft and camera anomalies due to the intense radiation. close
to Jupiter, there were many successful SSI observations during GMM.
Four giant, high-latitude plumes, including the largest plume ever
observed on to, were documented over a period of eight months; only
faint evidence of such plumes had been seen since the Voyager 2 encounter,
despite monitoring by Galileo during the previous five years. Moreover,
the source of one of the plumes was Tvashtar Catena, demonstrating
that a single site can exhibit remarkably diverse eruption styles-from
a curtain of lava fountains, to extensive surface flows, and finally
a similar to 400 km high plume-over a relatively short period of
time (similar to 13 months between orbits 125 and G29). Despite this
substantial activity, no evidence of any truly new volcanic center
was seen during the six years of Galileo observations. The recent
observations also revealed details of mass wasting processes acting
on to. Slumping and landsliding dominate and occur in close proximity
to each other, demonstrating spatial variation in material properties
over distances of several kilometers. However, despite the ubiquitous
evidence for mass wasting, the rate of volcanic resurfacing seems
to dominate; the floors of paterae in proximity to mountains are
generally free of debris. Finally, the highest resolution observations
obtained during Galileo's final encounters with to provided further
evidence for a wide diversity of surface processes at work on to.
(C) 2003 Elsevier Inc. All rights reserved.},
added-at = {2009-11-03T20:21:25.000+0100},
author = {Turtle, E. P. and Keszthelyi, L. P. and McEwen, A. S. and Radebaugh, J. and Milazzo, M. and Simonelli, D. P. and Geissler, P. and Williams, D. A. and Perry, J. and Jaeger, W. L. and Klaasen, K. P. and Breneman, H. H. and Denk, T. and Phillips, C. B.},
biburl = {https://www.bibsonomy.org/bibtex/24fa7010e32c813abbcc3f9b129b32f36/svance},
citedreferences = {ANDERSON JD, 2002, EOS T AGU FALL M S, V83 ; BART GD, 2004, Icarus, V169, P111 ; DAVIES AG, 2000, Icarus, V148, P211 ; DAVIES AG, 2001, J GEOPHYS RES-PLANET, V106, P33079 ; FIESELER PD, 2003, OBJECTS NEAR JUPITER, P8107 ; FRANK LA, 2001, J GEOPHYS RES-SPACE, V106, P26209 ; GEISSLER P, 2004, Icarus, V169, P29 ; GEISSLER PE, 1999, Icarus, V140, P265 ; Greeley R, 1984, Icarus, V60, P189 ; HELIKER C, 2003, US GEOL SURV PROF PA, V1676, P1 ; HOWELL RR, 2001, J GEOPHYS RES-PLANET, V106, P33129 ; JAEGER WL, 2000, EOS T AGU SPRING M S, V81 ; JAEGER WL, 2002, P LUN PLAN SCI C 33 ; JAEGER WL, 2003, J GEOPHYS RES, V108 ; JOHNSON TV, 1995, GEOPHYS RES LETT, V22, P3293 ; KESZTHELYI L, 2001, J GEOPHYS RES-PLANET, V106, P33025 ; KESZTHELYI L, 2004, Icarus, V169, P271 ; KLAASEN KP, 1997, OPT ENG, V36, P3001 ; KLAASEN KP, 2003, OPT ENG, V42, P494 ; LOPES RMC, 2001, J GEOPHYS RES-PLANET, V106, P33053 ; LOPES RMC, 2004, Icarus, V169, P140 ; LOPESGAUTIER R, 1999, Icarus, V140, P243 ; MARCHIS F, 2002, EOS T AGU FALL M S, V83 ; MATTOX TN, 1993, B VOLCANOL, V55, P407 ; MCEWEN AS, 1983, Icarus, V55, P191 ; 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 ; MCEWEN AS, 2003, FORUM JUPITER ICY MO ; MCEWEN AS, 2003, JUPITER PLANET STAEL ; MOORE JM, 2001, J GEOPHYS RES-PLANET, V106, P33223 ; NASH DB, 1987, Icarus, V72, P1 ; PERRY J, 2003, P LUN PLANT SCI C 34 ; PHILLIPS CB, 2000, THESIS U ARIZONA TUC ; PORCO CC, 2003, Science, V299, P1541 ; RADEBAUGH J, 2001, J GEOPHYS RES-PLANET, V106, P33005 ; RADEBAUGH J, 2004, Icarus, V169, P65 ; RATHBUN JA, 2002, GEOPHYS RES LETT, V29 ; SAGAN C, 1979, Nature, V280, P750 ; SCHABUN JA, 1982, SATELLITES JUPITER, P556 ; SCHENK P, 2001, J GEOPHYS RES-PLANET, V106, P33201 ; SCHENK PM, 1998, Science, V279, P1514 ; Schmitt B, 2003, J GEOPHYS RES, V108 ; SIMONELLI DP, 1997, GEOPHYS RES LETT, V24, P2475 ; SMITH BA, 1979, Science, V204, P951 ; SMYTHE WD, 2000, B AM ASTRON SOC, V32, P1047 ; SMYTHE WD, 2003, EOS T AGU FALL M S, V84 ; SPENCER JR, 2002, ASTRON SCO PAC C SER, V270, P201 ; SPENCER JR, 2003, EOS T AGU FALL M S, V84 ; THEILIG EE, 2002, 53 INT ASTR C ; TURTLE EP, 2001, J GEOPHYS RES-PLANET, V106, P33175 ; TURTLE EP, 2002, J GEOPHYS RES, V107 ; WATANABE T, 1940, JAP J GEOL GEOGR, V17, P289 ; WILLIAMS DA, 2001, J GEOPHYS RES-PLANET, V106, P33105 ; WILLIAMS DA, 2001, J GEOPHYS RES-PLANET, V106, P33161 ; WILLIAMS DA, 2002, J GEOPHYS RES, V107 ; WILLIAMS DA, 2002, P LUN PLAN SCI C 33 ; WILLIAMS DA, 2004, Icarus, V169, P80 ; WILSON L, 2001, J GEOPHYS RES-PLANET, V106, P32997},
interhash = {e893972d5880b80319c7ba478ce4acbb},
intrahash = {4fa7010e32c813abbcc3f9b129b32f36},
journal = {Icarus},
keywords = {ACTIVE CALIBRATION; EMPLACEMENT; ERUPTION; FLOW FLOWS; IO; JUPITERS MISSION; MOON MOUNTAINS; PLUMES SULFUR SYSTEM; VOLCANISM;},
number = 1,
owner = {svance},
pages = {3--28},
timestamp = {2009-11-03T20:22:19.000+0100},
title = {The final Galileo SSI observations of Io: orbits G28-I33},
volume = 169,
year = 2004
}