A close-up look at Io from Galileo's near-infrared mapping spectrometer

Science

Volumn 288, Issue 5469, 2000, Pages 1201-1204

  Lopes Gautier, Rosaly ^a   Doute S ^b   Smythe, W D ^a   Kamp, L W ^a   Carlson, R W ^a   Davies, A G ^a   Leader, F E ^b   McEwen, A S ^d   Geissler, P E ^d   Kieffer, S W ^c   Keszthelyi, L ^d   Barbinis, E ^a   Mehlman, R ^b   Segura, M ^a   Shirley, J ^a   Soderblom, L A ^e  

^a CALIFORNIA INSTITUTE OF TECHNOLOGY   (United States)

^b UNIVERSITY OF CALIFORNIA   (United States)

^c S W Kieffer Sci Consulting Inc   (Canada)

^d UNIVERSITY OF ARIZONA   (United States)

^e U S GEOLOGICAL SURVEY   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

SULFUR DIOXIDE;

IO; SULFUR DIOXIDE; THERMAL STRUCTURE; VOLCANO;

ARTICLE; IMAGE DISPLAY; INFRARED SPECTROMETRY; PLUME; PRIORITY JOURNAL; SPACE FLIGHT; SPECTRAL SENSITIVITY; TEMPERATURE MEASUREMENT; VOLCANO;

FLIGHT EXPERIMENT; GALILEO PROJECT; LONG DURATION; UNMANNED;

EXTRATERRESTRIAL ENVIRONMENT; HEAT; JUPITER; SPACECRAFT; SPECTROSCOPY, NEAR-INFRARED; SUNLIGHT; TEMPERATURE; VOLCANIC ERUPTION;

EID: 0034685938     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.288.5469.1201     Document Type: Article

References (24)

1. R. Lopes-Gautier et al., Icarus 140, 243 (1999).
2. R. W. Carlson et al., Geophys. Res. Lett. 24, 2479 (1997).
3. S. Douté et al., in preparation.
4. P. E. Goissler et al., Icarus 140, 265 (1999).
5. R. G. Strom and N. M. Schneider, in Satellites of Jupiter, D. Morrison, Ed. (Univ. of Arizona Press, Tucson, AZ, 1982), pp. 598-633, and references therein.
6. Web fig. 1 is available at www.sciencemag.org/ feature/data/1049493.shl
7. A. G. Davies et al., Lunar Planet. Sci. XXX (1999) [CD-ROM].
8. B < 200 K were not used in this analysis.
9. The relative band depth is defined as the ratio [A(3.0)/ A(4.1)], where A(λ) is the measured albedo (reflectance) at wavelength λ. This ratio was not obtained for pixels in which thermal emission could be detected.
10. B. Schmitt et al., Icarus 111, 79 (1994); B. Schmitt et al., in Solar System Ices, B. Schmitt, C. De Bergh, M. Festou, Eds. (Kluwer Academic, Dordrecht, Netherlands, 1998), pp. 199-240.
11. B. Schmitt et al., Icarus 111, 79 (1994); B. Schmitt et al., in Solar System Ices, B. Schmitt, C. De Bergh, M. Festou, Eds. (Kluwer Academic, Dordrecht, Netherlands, 1998), pp. 199-240.
12. 2 distribution maps of S. Douté et al. (3), which modeled 408-wavelength NIMS spectra.
13. J. R. Spencer et al., Science 288, 1208 (2000).
14. Times calculated using the model of A. C. Davies [Icarus 124, 45 (1996)]. These temperatures and cooling rates assume that the surface heat loss is buffered by the release of latent heat from a stillmolten flow interior.
15. R. Howell et al., Lunar Planet. Sci. XXXI (2000) [CD-ROM].
16. A. S. McEwen et al., Science 288, 1193 (2000).
17. A. S. McEwen et al., Science 281, 87 (1998).
18. A. S. McEwen et al., Icarus 135, 181 (1998).
19. S. W. Kieffer et al., Science 288, 1204 (2000).
20. Previously undetected hot spots detected by NIMS during 124 and 125 are located at (+21, 146W, near Surya), (+14, 150 W), (+20, 149W), (+12, 158W, near Chaac), (-5, 132W, the dark feature Seth), and (+9, 133W)
21. J. C. Pearl and W. M. Sinton, in (5), pp. 724-755.
22. J. R. Spencer et al., Icarus 127, 221 (1997).
23. The pixel size in NIMS-processed images is 0.5X the instrument's spatial resolution.
24. Portions of this work were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.