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J. Veverka,1M. Robinson,2P. Thomas,1S. Murchie,3J. F. Bell III,1N. Izenberg,3C. Chapman,4A. Harch,1M. Bell,1B. Carcich,1A. Cheng,3B. Clark,1D. Domingue,3D. Dunham,3R. Farquhar,3M. J. Gaffey,5E. Hawkins,3J. Joseph,1R. Kirk,6H. Li,2P. Lucey,7M. Malin,8P. Martin,1L. McFadden,9W. J. Merline,4J. K. Miller,10W. M. Owen Jr.,10C. Peterson,1L. Prockter,3J. Warren,3D. Wellnitz,9B. G. Williams,10D. K. Yeomans10
Eros is a very elongated (34 kilometers by 11 kilometers
by 11 kilometers) asteroid, most of the surface of which is saturatedwith craters smaller than 1 kilometer in diameter. The largestcrater
is 5.5 kilometers across, but there is a 10-kilometer saddle-likedepression with attributes of a large degraded crater. Surfacelineations, both grooves and ridges, are prominent on Eros; someprobably exploit planes of weakness produced by collisions onEros
and/or its parent body. Ejecta blocks (30 to 100 meters across)are
abundant but not uniformly distributed over the surface. Albedovariations are restricted to the inner walls of certain cratersand may
be related to downslope movement of regolith. On scalesof 200 meters
to 1 kilometer, Eros is more bland in terms of colorvariations than
Gaspra or Ida. Spectra (800 to 2500 nanometers)are consistent with an
ordinary chondrite composition for whichthe measured mean density of
2.67 ± 0.1 grams per cubic centimeterimplies internal porosities
ranging from about 10 to 30 percent.
1 Space Sciences Building, Cornell University,
Ithaca, NY 14853, USA.
2 Department of Geological
Sciences, Northwestern University, 309 Locy Hall, Evanston, IL 60208, USA.
3 Applied Physics Laboratory, Johns Hopkins
University, 1110 Johns Hopkins Road, Laurel, MD 20723, USA.
4 Southwest Research Institute, 1050 Walnut Street,
Suite 426, Boulder, CO 80302, USA.
5 Department of
Earth and Environmental Sciences, Science Center, Rensselaer
Polytechnic Institute, 110 8th Street, Troy, NY 12180-3590, USA.
6 U.S. Geological Survey, 2255 North Gemini Drive,
Flagstaff, AZ 86001, USA.
7 University of Hawaii,
Hawaii Institute of Geophysics and Planetology, 2525 Correa Road,
Honolulu, HI 96822, USA.
8 Malin Space Science
Systems, Post Office Box 910148, San Diego, CA 92191, USA.
9 Department of Astronomy, University of Maryland,
College Park, MD 20742, USA.
10 Jet Propulsion
Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA.
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In Science Magazine
PERSPECTIVES
Richard P. Binzel (22 September 2000) Science289 (5487), 2065.
[DOI: 10.1126/science.289.5487.2065] |Summary »|Full Text »
REPORTS
D. K. Yeomans, P. G. Antreasian, J.-P. Barriot, S. R. Chesley, D. W. Dunham, R. W. Farquhar, J. D. Giorgini, C. E. Helfrich, A. S. Konopliv, J. V. McAdams, J. K. Miller, W. M. Owen, Jr., D. J. Scheeres, P. C. Thomas, J. Veverka, and B. G. Williams (22 September 2000) Science289 (5487), 2085.
[DOI: 10.1126/science.289.5487.2085] |Abstract »|Full Text »|PDF »
REPORTS
Maria T. Zuber, David E. Smith, Andrew F. Cheng, James B. Garvin, Oded Aharonson, Timothy D. Cole, Peter J. Dunn, Yanping Guo, Frank G. Lemoine, Gregory A. Neumann, David D. Rowlands, and Mark H. Torrence (22 September 2000) Science289 (5487), 2097.
[DOI: 10.1126/science.289.5487.2097] |Abstract »|Full Text »|PDF »
REPORTS
J. I. Trombka, S. W. Squyres, J. Brückner, W. V. Boynton, R. C. Reedy, T. J. McCoy, P. Gorenstein, L. G. Evans, J. R. Arnold, R. D. Starr, L. R. Nittler, M. E. Murphy, I. Mikheeva, R. L. McNutt, Jr., T. P. McClanahan, E. McCartney, J. O. Goldsten, R. E. Gold, S. R. Floyd, P. E. Clark, T. H. Burbine, J. S. Bhangoo, S. H. Bailey, and M. Petaev (22 September 2000) Science289 (5487), 2101.
[DOI: 10.1126/science.289.5487.2101] |Abstract »|Full Text »|PDF »
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