Pele has been the most intense high-temperature hotspot on Io to be
continuously active during the Galileo monitoring from 1996-2001.
A suite of characteristics suggests that Pele is an active lava lake
inside a volcanic depression. In 2000-2001, Pele was observed by
two spacecraft, Cassini and Galileo. The Cassini observations revealed
that Pele is variable in activity over timescales of minutes, typical
of active lava lakes in Hawaii and Ethiopia. These observations also
revealed that the short-wavelength thermal emission from Pele decreases
with rotation of Io by a factor significantly greater than the cosine
of the emission angle, and that the color temperature becomes more
variable and hotter at high emission angles. This behavior suggests
that a significant portion of the visible thermal emission from Pele
comes from lava fountains within a topographically confined lava
body. High spatial resolution, nightside images from a Galileo flyby
in October 2001 revealed a large, relatively cool (< 800 K) region,
ringed by bright hotspots, and a central region of high thermal emission,
which is hypothesized to be due to fountaining and convection in
the lava lake. Images taken through different filters revealed color
temperatures of 1500 +/- 80 K from Cassini ISS data and 1605 +/-
220 and 14120 +/- 100 K from small portions of Galileo SSI data.
Such temperatures are near the upper limit for basaltic compositions.
Given the limitations of deriving lava eruption temperature in the
absence of in situ measurement, it is possible that Pele has lavas
with ultramafic compositions. The long-lived, vigorous activity of
what is most likely an actively overturning lava lake in Pele Patera
indicates that there is a strong connection to a large, stable magma
source region. (C) 2003 Elsevier Inc. All rights reserved.
%0 Journal Article
%1 Radebaugh2004
%A Radebaugh, J.
%A McEwen, A. S.
%A Milazzo, M. P.
%A Keszthelyi, L. P.
%A Davies, A. G.
%A Turtle, E. P.
%A Dawson, D. D.
%D 2004
%J Icarus
%K ACTIVE EMISSION; ERUPTION; HOT-SPOTS; IO; JUPITERS LAKE; LAVA LITHOSPHERE MISSION; MOON PLUME; SILICATE THERMAL VOLCANISM;
%N 1
%P 65--79
%T Observations and temperatures of Io's Pele Patera from Cassini and Galilee spacecraft images
%V 169
%X Pele has been the most intense high-temperature hotspot on Io to be
continuously active during the Galileo monitoring from 1996-2001.
A suite of characteristics suggests that Pele is an active lava lake
inside a volcanic depression. In 2000-2001, Pele was observed by
two spacecraft, Cassini and Galileo. The Cassini observations revealed
that Pele is variable in activity over timescales of minutes, typical
of active lava lakes in Hawaii and Ethiopia. These observations also
revealed that the short-wavelength thermal emission from Pele decreases
with rotation of Io by a factor significantly greater than the cosine
of the emission angle, and that the color temperature becomes more
variable and hotter at high emission angles. This behavior suggests
that a significant portion of the visible thermal emission from Pele
comes from lava fountains within a topographically confined lava
body. High spatial resolution, nightside images from a Galileo flyby
in October 2001 revealed a large, relatively cool (< 800 K) region,
ringed by bright hotspots, and a central region of high thermal emission,
which is hypothesized to be due to fountaining and convection in
the lava lake. Images taken through different filters revealed color
temperatures of 1500 +/- 80 K from Cassini ISS data and 1605 +/-
220 and 14120 +/- 100 K from small portions of Galileo SSI data.
Such temperatures are near the upper limit for basaltic compositions.
Given the limitations of deriving lava eruption temperature in the
absence of in situ measurement, it is possible that Pele has lavas
with ultramafic compositions. The long-lived, vigorous activity of
what is most likely an actively overturning lava lake in Pele Patera
indicates that there is a strong connection to a large, stable magma
source region. (C) 2003 Elsevier Inc. All rights reserved.
@article{Radebaugh2004,
abstract = {Pele has been the most intense high-temperature hotspot on Io to be
continuously active during the Galileo monitoring from 1996-2001.
A suite of characteristics suggests that Pele is an active lava lake
inside a volcanic depression. In 2000-2001, Pele was observed by
two spacecraft, Cassini and Galileo. The Cassini observations revealed
that Pele is variable in activity over timescales of minutes, typical
of active lava lakes in Hawaii and Ethiopia. These observations also
revealed that the short-wavelength thermal emission from Pele decreases
with rotation of Io by a factor significantly greater than the cosine
of the emission angle, and that the color temperature becomes more
variable and hotter at high emission angles. This behavior suggests
that a significant portion of the visible thermal emission from Pele
comes from lava fountains within a topographically confined lava
body. High spatial resolution, nightside images from a Galileo flyby
in October 2001 revealed a large, relatively cool (< 800 K) region,
ringed by bright hotspots, and a central region of high thermal emission,
which is hypothesized to be due to fountaining and convection in
the lava lake. Images taken through different filters revealed color
temperatures of 1500 +/- 80 K from Cassini ISS data and 1605 +/-
220 and 14120 +/- 100 K from small portions of Galileo SSI data.
Such temperatures are near the upper limit for basaltic compositions.
Given the limitations of deriving lava eruption temperature in the
absence of in situ measurement, it is possible that Pele has lavas
with ultramafic compositions. The long-lived, vigorous activity of
what is most likely an actively overturning lava lake in Pele Patera
indicates that there is a strong connection to a large, stable magma
source region. (C) 2003 Elsevier Inc. All rights reserved.},
added-at = {2009-11-03T20:21:25.000+0100},
author = {Radebaugh, J. and McEwen, A. S. and Milazzo, M. P. and Keszthelyi, L. P. and Davies, A. G. and Turtle, E. P. and Dawson, D. D.},
biburl = {https://www.bibsonomy.org/bibtex/2f806fa00ae612c633920aef38878a4c1/svance},
citedreferences = {BURGI PY, 2002, B VOLCANOL, V64, P472 ; CARR MH, 1979, Nature, V280, P729 ; CARR MH, 1986, J GEOPHYS RES-SOLID, V91, P3521 ; CARR MH, 1998, Icarus, V135, P146 ; DAVIES AG, 1996, Icarus, V124, P45 ; DAVIES AG, 2001, J GEOPHYS RES-PLANET, V106, P33079 ; DAVIES AG, 2002, P LUN PLAN SCI C 33 ; DAVIES AG, 2003, IN PRESS GEOPHYS RES ; FLYNN LP, 1993, J GEOPHYS RES-SOLID, V98, P6461 ; GEISSLER PE, 1999, Icarus, V140, P265 ; HARRIS AJL, 1999, J GEOPHYS RES-SOL EA, V104, P7117 ; HOWELL RR, 1997, Icarus, V127, P394 ; JAEGER WL, 2003, J GEOPHYS RES, V108, P5094 ; JOHNSON TV, 1982, SATELLITES JUPITER, P634 ; JOHNSON TV, 1995, GEOPHYS RES LETT, V22, P3293 ; KARGEL JS, 2003, EOS, V84, P313 ; KESZTHELYI L, 1997, Icarus, V130, P437 ; KESZTHELYI L, 2001, J GEOPHYS RES-PLANET, V106, P33025 ; KESZTHELYI L, 2004, Icarus, V169, P271 ; KIEFFER SW, 2000, Science, V288, P1204 ; KLAASEN KP, 1997, OPT ENG, V36, P3001 ; LOPES RMC, 2001, J GEOPHYS RES-PLANET, V106, P33053 ; LOPES RMC, 2004, Icarus, V169, P140 ; LOPESGAUTIER R, 1999, Icarus, V140, P243 ; MARCHIS F, 2001, J GEOPHYS RES-PLANET, V106, P33141 ; 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 ; MCKINNON WB, 2001, Geology, V29, P103 ; MILAZZO MP, 2001, J GEOPHYS RES-PLANET, V106, P33121 ; MINER ED, 2002, ASTR SOC P, V281, P373 ; OREILLY TC, 1981, GEOPHYS RES LETT, V8, P313 ; PEARL JC, 1982, SATELLITES JUPITER, P724 ; PHILLIPS CB, 2000, THESIS U ARIZONA TUS ; PIKE RJ, 1981, 811038 US GEOL SURV ; PORCO CC, 2003, Science, V299, P1541 ; RADEBAUGH J, 1999, THESIS BRIGHAM YOUNG ; RADEBAUGH J, 2001, AAS DPS M 33 ; RADEBAUGH J, 2001, J GEOPHYS RES-PLANET, V106, P33005 ; RADEBAUGH J, 2002, EOS T AGU SPR M S, V83, P33005 ; RATHBUN JA, 2004, Icarus, V169, P127 ; SCHENK PM, 1998, Science, V279, P1514 ; SMITH BA, 1979, Science, V204, P951 ; SPENCER JR, 1996, ANNU REV EARTH PL SC, V24, P125 ; SPENCER JR, 1997, GEOPHYS RES LETT, V24, P2471 ; SPENCER JR, 1997, Icarus, V127, P221 ; SPENCER JR, 2000, Science, V288, P1198 ; SPENCER JR, 2000, Science, V288, P1208 ; STANSBERRY JA, 1999, P LUN PLAN SCI C 30 ; STARK PB, 1997, STICI GUI STAT TOOLS ; STROM RG, 1979, Nature, V280, P733 ; STROM RG, 1981, J GEOPHYS RES, V86, P8593 ; TURTLE EP, 2001, J GEOPHYS RES, V106, P33173 ; TURTLE EP, 2004, Icarus, V169, P3 ; WILLIAMS DA, 2001, J GEOPHYS RES-PLANET, V106, P33105 ; WRIGHT TL, 1977, 1004 US GEOL SURV ; ZHANG Q, 2002, P LUN PLAN SCI C 33 ; ZOLOTOV MY, 2000, GEOPHYS RES LETT, V27, P2789},
interhash = {af053c6fd39d7c23f79375b216115cc8},
intrahash = {f806fa00ae612c633920aef38878a4c1},
journal = {Icarus},
keywords = {ACTIVE EMISSION; ERUPTION; HOT-SPOTS; IO; JUPITERS LAKE; LAVA LITHOSPHERE MISSION; MOON PLUME; SILICATE THERMAL VOLCANISM;},
number = 1,
owner = {svance},
pages = {65--79},
timestamp = {2009-11-03T20:22:11.000+0100},
title = {Observations and temperatures of Io's Pele Patera from Cassini and Galilee spacecraft images},
volume = 169,
year = 2004
}