During the Cassini-Jupiter flyby, VIMS observed Io at different phase
angles, both in full sunlight and in eclipse. By using the sunlight
measurements, we were able to produce phase curves in the visual
through all the near infrared wavelengths covered by the VIMS instrument
(0.85-5.1 mum). The phase angle spanned from similar to2degrees to
similar to120degrees. The measurements, done just after To emerged
from Jupiter's shadow, show an increase of about 15% in Io's reflectance
with respect to what would be predicted by the phase curve. This
behavior is observed at wavelengths > 1.2 mum. Moreover, just after
emergence from eclipse an increase of about 25% is observed in the
depth of SO2 frost bands at 4.07 and 4.35 mum. At 0.879 < lambda
< 1.04 mum the brightening is 10-24%. Below lambda = 0.879 mum the
brightening, if present, should be less than the precision of our
measurements (similar to5%). Apparently, these observations are not
explained neither by a diverse spatial distribution of SO2 on the
Io' surface nor by atmospheric SO2 condensation on the surface during
the eclipse. (C) 2004 Elsevier Inc. All rights reserved.
%0 Journal Article
%1 Bellucci2004
%A Bellucci, G.
%A D'Aversa, E.
%A Formisano, V.
%A Cruikshank, D.
%A Nelson, R. M.
%A Clark, R. N.
%A Baines, K. H.
%A Matson, D.
%A Brown, R. H.
%A McCord, T. B.
%A Buratti, B. J.
%A Nicholson, P. D.
%D 2004
%J Icarus
%K ALBEDO ATMOSPHERE; BIDIRECTIONAL CHANGES; CONDENSATION; INFRARED JUPITER; LO; MAPPING NIGHTSIDE; REFLECTANCE SEARCH; SPECTROMETER; SPECTROSCOPY; VIMS
%N 1
%P 141--148
%T Cassini/VIMS observation of an Io post-eclipse brightening event
%V 172
%X During the Cassini-Jupiter flyby, VIMS observed Io at different phase
angles, both in full sunlight and in eclipse. By using the sunlight
measurements, we were able to produce phase curves in the visual
through all the near infrared wavelengths covered by the VIMS instrument
(0.85-5.1 mum). The phase angle spanned from similar to2degrees to
similar to120degrees. The measurements, done just after To emerged
from Jupiter's shadow, show an increase of about 15% in Io's reflectance
with respect to what would be predicted by the phase curve. This
behavior is observed at wavelengths > 1.2 mum. Moreover, just after
emergence from eclipse an increase of about 25% is observed in the
depth of SO2 frost bands at 4.07 and 4.35 mum. At 0.879 < lambda
< 1.04 mum the brightening is 10-24%. Below lambda = 0.879 mum the
brightening, if present, should be less than the precision of our
measurements (similar to5%). Apparently, these observations are not
explained neither by a diverse spatial distribution of SO2 on the
Io' surface nor by atmospheric SO2 condensation on the surface during
the eclipse. (C) 2004 Elsevier Inc. All rights reserved.
@article{Bellucci2004,
abstract = {During the Cassini-Jupiter flyby, VIMS observed Io at different phase
angles, both in full sunlight and in eclipse. By using the sunlight
measurements, we were able to produce phase curves in the visual
through all the near infrared wavelengths covered by the VIMS instrument
(0.85-5.1 mum). The phase angle spanned from similar to2degrees to
similar to120degrees. The measurements, done just after To emerged
from Jupiter's shadow, show an increase of about 15% in Io's reflectance
with respect to what would be predicted by the phase curve. This
behavior is observed at wavelengths > 1.2 mum. Moreover, just after
emergence from eclipse an increase of about 25% is observed in the
depth of SO2 frost bands at 4.07 and 4.35 mum. At 0.879 < lambda
< 1.04 mum the brightening is 10-24%. Below lambda = 0.879 mum the
brightening, if present, should be less than the precision of our
measurements (similar to5%). Apparently, these observations are not
explained neither by a diverse spatial distribution of SO2 on the
Io' surface nor by atmospheric SO2 condensation on the surface during
the eclipse. (C) 2004 Elsevier Inc. All rights reserved.},
added-at = {2009-11-03T20:21:25.000+0100},
author = {Bellucci, G. and D'Aversa, E. and Formisano, V. and Cruikshank, D. and Nelson, R. M. and Clark, R. N. and Baines, K. H. and Matson, D. and Brown, R. H. and McCord, T. B. and Buratti, B. J. and Nicholson, P. D.},
biburl = {https://www.bibsonomy.org/bibtex/2f35412d9bfc8b20697ed33157d52f44b/svance},
citedreferences = {ABRAMENKO AN, 1976, ASTRON VESTN, V10, P195 ; BAUM WA, 1953, ASTRON J, V58, P108 ; BINDER AB, 1964, Icarus, V3, P299 ; BROWN RH, 2003, Icarus, V164, P461 ; BURATTI BJ, 1995, Icarus, V118, P418 ; CRUIKSHANK DP, 1973, Icarus, V20, P7 ; DOMINGUE DL, 1998, Icarus, V134, P113 ; DOUTE S, 2001, Icarus, V149, P107 ; FALLON FW, 1971, Icarus, V15, P492 ; FANALE FP, 1981, GEOPHYS RES LETT, V8, P625 ; FORMISANO V, 2003, Icarus, V166, P75 ; FRANZ OG, 1971, Icarus, V14, P13 ; FRANZ OG, 1974, Icarus, V23, P431 ; HAMMEL HB, 1985, Icarus, V64, P125 ; HAPKE B, 1984, Icarus, V59, P41 ; HAPKE B, 1986, Icarus, V67, P264 ; JOHNSON TV, 1971, Icarus, V14, P94 ; MCCORD TB, 2004, Icarus, V172, P104 ; MILLER E, 1996, P SOC PHOTO-OPT INS, V2803, P206 ; MILLIS RL, 1974, Icarus, V23, P425 ; NASH DB, 1995, Icarus, V117, P402 ; NELSON RM, 1977, Icarus, V32, P225 ; NELSON RM, 1978, Icarus, V33, P203 ; NELSON RM, 1993, Icarus, V101, P223 ; NELSON RM, 1996, Icarus, V101, P223 ; OLEARY BT, 1971, Icarus, V14, P265 ; OLEARY BT, 1973, Icarus, V20, P18 ; OSHAUGHNESSY M, 1989, LUNAR PLANET SCI, V20, P812 ; PAVLOVSKI K, 1976, Icarus, V29, P509 ; REININGER F, 1994, P SOC PHOTO-OPT INS, V2198, P239 ; SECOSKY JJ, 1994, Icarus, V111, P73 ; SIMONELLI DP, 1994, Icarus, V107, P375 ; SIMONELLI DP, 1998, Icarus, V135, P166 ; STROBEL DF, 2001, ASTROPHYS SPACE SCI, V277, P271 ; VEVERKA J, 1981, Icarus, V47, P60 ; WASSERMAN LH, 1973, Icarus, V20, P322},
interhash = {014a9d11eed5184044623162333b6b50},
intrahash = {f35412d9bfc8b20697ed33157d52f44b},
journal = {Icarus},
keywords = {ALBEDO ATMOSPHERE; BIDIRECTIONAL CHANGES; CONDENSATION; INFRARED JUPITER; LO; MAPPING NIGHTSIDE; REFLECTANCE SEARCH; SPECTROMETER; SPECTROSCOPY; VIMS},
number = 1,
owner = {svance},
pages = {141--148},
timestamp = {2009-11-03T20:21:39.000+0100},
title = {Cassini/VIMS observation of an Io post-eclipse brightening event},
volume = 172,
year = 2004
}