Smith, Bradford A. and Soderblom, Laurence A. and Beebe, Reta and Boyce, Joseph and Briggs, Geoffrey and Carr, Michael and Collins, Stewart A. and Cook, Allan F., II and Danielson, G. Edward and Davies, Merton E. and Hunt, Garry E. and Ingersoll, Andrew and Johnson, Torrence V. and Masursky, Harold and McCauley, John and Morrison, David and Owen, Tobias and Sagan, Carl and Shoemaker, Eugene M. and Strom, Robert and Suomi, Verner E. and Veverka, Joseph (1979) The Galilean Satellites and Jupiter: Voyager 2 Imaging Science Results. Science, 206 (4421). pp. 927-950. ISSN 0036-8075. https://resolver.caltech.edu/CaltechAUTHORS:20130129-140114720
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Abstract
Voyager 2, during its encounter with the Jupiter system, provided images that both complement and supplement in important ways the Voyager 1 images. While many changes have been observed in Jupiter's visual appearance, few, yet significant, changes have been detected in the principal atmospheric currents. Jupiter's ring system is strongly forward scattering at visual wavelengths and consists of a narrow annulus of highest particle density, within which is a broader region in which the density is lower. On Io, changes are observed in eruptive activity, plume structure, and surface albedo patterns. Europa's surface retains little or no record of intense meteorite bombardment, but does reveal a complex and, as yet, little-understood system of overlapping bright and dark linear features. Ganymede is found to have at least one unit of heavily cratered terrain on a surface that otherwise suggests widespread tectonism. Except for two large ringed basins, Callisto's entire surface is heavily cratered.
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| Additional Information: | © 1979 American Association for the Advancement of Science. Received for publication 26 September 1979. Several of the observations reported here were possible only because the Voyager Project Office permitted major, last-minute redesign of Voyager 2's near-encounter command load to increase observations of various features discovered by Voyager 1. Many individuals contributed significantly to this successful effort, with J. S. Carter, C. J. Hansen, W. A. Magoon and S. J. Zawacki playing key roles. The success of this experiment is a tribute to the extraordinary efforts of the hundreds of individuals, throughout the world, who have devoted their considerable talents to this undertaking. Among those who contributed most directly to the Voyager 2 Jupiter imaging operations are: J. L. Mitchell (Jupiter observational design and subsequent velocity measurement); P. N. Kupferman (exposure determination); J. L. Anderson, A. L. Lane, C. H. Stembridgea, nd the personnel of the Voyager Sequence Team and the Mission Imaging Operations Group (data acquisition and processing); C. C. Avis, G. W. Garneau, P. L. Jepsen, E. P. Korsmo, J. A. Mosher, A. A. Schwartz, and G. M. Yagi (image processing); R. Batson, P. Bridges, P. Collins, J. Inge, C. Isbell, B. K. Luchitta, D. C. Pieri, G. G. Schaber, and R. Tyner (analysis and cartography); R. Gurrola, J. T. Harwood, V. J. Nelson, L. J. Pieri, F. Popescu, D. Simonelli, and the Jet Propulsion Laboratory (JPL) Photolab (operational support); and M. J. S. Belton, M. Flasar, H. Kieffer, M. C. Malin, and R. J. Terrile for their careful reviews of this manuscript. G. E. Hunt is supported by the Science Research Council, Great Britain. This is contribution 3325 of the Division of Geological and Planetary Sciences, California Institute of Technology. This report presents the results of one phase of research carried out at JPL under NASA contract NAS 7-100. | |||||||||
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| Issue or Number: | 4421 | |||||||||
| Record Number: | CaltechAUTHORS:20130129-140114720 | |||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20130129-140114720 | |||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | |||||||||
| ID Code: | 36661 | |||||||||
| Collection: | CaltechAUTHORS | |||||||||
| Deposited By: | Jason Perez | |||||||||
| Deposited On: | 30 Jan 2013 19:20 | |||||||||
| Last Modified: | 03 Oct 2019 04:40 |
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