%0 Journal Article %1 Hansen2004 %A Hansen, G. B. %A McCord, T. B. %D 2004 %J Journal of Geophysical Research-Planets %K H2O HYDRATED ICE; IH; MINERALS; NEAR-INFRARED OPTICAL-CONSTANTS; PHOTOPOLARIMETER-RADIOMETER; SALT SOLID SPECTRA; SURFACE TEMPERATURE; WATER-ICE; WATER; %N E1 %P E01012 %T Amorphous and crystalline ice on the Galilean satellites: A balance between thermal and radiolytic processes %V 109 %X 1 The water ice on the three outermost Galilean satellites of Jupiter has a lattice structure that can vary from crystalline to amorphous. Amorphous ice is crystallized by heating, while crystalline ice is amorphized through disruption by particle radiation. We determine ice lattice order using infrared spectra from the Near Infrared Mapping Spectrometer on the Galileo Jupiter orbiter. The shape of the reflectance peak near 3.1 mum is diagnostic of the lattice order in the top micrometers of the surface. A narrow, temperature-sensitive band near 1.65 mum, from similar to1 mm depth, is missing for amorphous ice. Spectral averages of > 100 pixels were used for Europa and Callisto, because of high radiation noise and small ice amounts, respectively. Model comparisons show that the surface ice is predominantly amorphous on Europa and predominantly crystalline on Callisto, while both types of ice are found on Ganymede. The distribution of Ganymede ice properties shows a broad global pattern of more amorphous ice in the high-latitude Jovian-facing hemisphere and in the low-latitude trailing hemisphere. The ice at similar to1 mm depth on all three satellites is predominantly crystalline. The radiation flux increases by similar to 300 times between Callisto and Europa, while the thermal crystallization rate may vary over five orders of magnitude among the three satellites ( being the fastest at Callisto). The occurrence of crystalline and amorphous ice suggests a balance between the disruption and crystallization, with Callisto dominated by thermal crystallization and Europa by radiative disruption, and with nearly equal rates between the two processes at Ganymede.

@article{Hansen2004, abstract = {[1] The water ice on the three outermost Galilean satellites of Jupiter has a lattice structure that can vary from crystalline to amorphous. Amorphous ice is crystallized by heating, while crystalline ice is amorphized through disruption by particle radiation. We determine ice lattice order using infrared spectra from the Near Infrared Mapping Spectrometer on the Galileo Jupiter orbiter. The shape of the reflectance peak near 3.1 mum is diagnostic of the lattice order in the top micrometers of the surface. A narrow, temperature-sensitive band near 1.65 mum, from similar to1 mm depth, is missing for amorphous ice. Spectral averages of > 100 pixels were used for Europa and Callisto, because of high radiation noise and small ice amounts, respectively. Model comparisons show that the surface ice is predominantly amorphous on Europa and predominantly crystalline on Callisto, while both types of ice are found on Ganymede. The distribution of Ganymede ice properties shows a broad global pattern of more amorphous ice in the high-latitude Jovian-facing hemisphere and in the low-latitude trailing hemisphere. The ice at similar to1 mm depth on all three satellites is predominantly crystalline. The radiation flux increases by similar to 300 times between Callisto and Europa, while the thermal crystallization rate may vary over five orders of magnitude among the three satellites ( being the fastest at Callisto). The occurrence of crystalline and amorphous ice suggests a balance between the disruption and crystallization, with Callisto dominated by thermal crystallization and Europa by radiative disruption, and with nearly equal rates between the two processes at Ganymede.}, added-at = {2009-11-03T20:21:25.000+0100}, author = {Hansen, G. B. and McCord, T. B.}, biburl = {https://www.bibsonomy.org/bibtex/2a4139f626d4865d36de1a368ac9e744a/svance}, citedreferences = {BARATTA GA, 1994, PLANET SPACE SCI, V42, P759 ; BERGREN MS, 1978, J CHEM PHYS, V69, P3477 ; BERTIE JE, 1964, J CHEM PHYS, V40, P1637 ; BERTIE JE, 1967, J CHEM PHYS, V46, P1271 ; BERTIE JE, 1969, J CHEM PHYS, V50, P4501 ; CALVIN WM, 1991, Icarus, V89, P305 ; CARLSON R, 1996, Science, V274, P385 ; CARLSON RW, 1992, SPACE SCI REV, V60, P457 ; CLAPP ML, 1995, J PHYS CHEM-US, V99, P6317 ; CLARK RN, 1982, Icarus, V49, P244 ; CLARK RN, 1986, SATELLITES, P437 ; CLARKE R, 2000, DAIRY IND INT, V65, P5 ; COOPER JF, 2001, Icarus, V149, P133 ; GRUNDY WM, 1998, J GEOPHYS RES-PLANET, V103, P25809 ; GRUNDY WM, 1999, Icarus, V142, P536 ; HAGEN W, 1981, CHEM PHYS, V56, P367 ; HANDA YP, 1988, CAN J CHEM, V66, P919 ; HANSEN GB, 2000, LUNAR PLANET SCI, V31 ; HANSEN GB, 2001, GEOPH RES ABSTR, V3, P7465 ; HARDIN AH, 1973, SPECTROCHIM ACTA A, V29, P1139 ; JENNISKENS P, 1998, SOLAR SYSTEM ICES, P199 ; JOHNSON RE, 1997, Icarus, V128, P469 ; JOHNSON TV, 1971, ASTROPHYS J, V169, P589 ; KOUCHI A, 1994, ASTRON ASTROPHYS, V290, P1009 ; KUIPER GP, 1961, PLANETS SATELLITES, P575 ; MASTRAPA RME, 2002, B AM ASTRON SOC, V34, P881 ; MATSON DL, 1989, Icarus, V77, P67 ; MCCORD TB, 1998, J GEOPHYS RES-PLANET, V103, P8603 ; MCCORD TB, 1999, J GEOPHYS RES-PLANET, V104, P11827 ; MCCORD TB, 1999, J GEOPHYS RES-PLANET, V104, P27157 ; MCCORD TB, 2001, Science, V292, P1523 ; MOORE JM, 1999, Icarus, V140, P294 ; MOROZ VI, 1965, ASTRON ZH, V42, P1287 ; ORTON GS, 1996, Science, V274, P389 ; PILCHER CB, 1972, Science NY, V178, P1087 ; POLLACK JB, 1978, Icarus, V36, P271 ; ROUSH TL, 1990, Icarus, V86, P355 ; ROUX JA, 1979, AEDCTR7957 ; Schmitt B, 1998, SOLAR SYSTEM ICES, P199 ; SILL GT, 1982, SATELLITES JUPITER, P174 ; SPENCER JR, 1987, Icarus, V69, P297 ; SPENCER JR, 1999, Science, V284, P1514 ; STRAZZULLA G, 1992, EUROPHYS LETT, V18, P517 ; TOON OB, 1994, J GEOPHYS RES-ATMOSP, V99, P25631 ; WARREN SG, 1984, APPL OPTICS, V23, P1206 ; WISCOMBE WJ, 1980, J ATMOS SCI, V37, P2712 ; WOOD BE, 1982, J OPT SOC AM, V72, P720}, interhash = {2bbba808d33bb1429c076e6ce87209cc}, intrahash = {a4139f626d4865d36de1a368ac9e744a}, journal = {Journal of Geophysical Research-Planets}, keywords = {H2O HYDRATED ICE; IH; MINERALS; NEAR-INFRARED OPTICAL-CONSTANTS; PHOTOPOLARIMETER-RADIOMETER; SALT SOLID SPECTRA; SURFACE TEMPERATURE; WATER-ICE; WATER;}, number = {E1}, owner = {svance}, pages = {E01012}, timestamp = {2009-11-03T20:21:50.000+0100}, title = {Amorphous and crystalline ice on the Galilean satellites: A balance between thermal and radiolytic processes}, volume = 109, year = 2004 }