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- C. T. Russell
- Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA 90095–1567, USA.
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- C. A. Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
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- A. Coradini
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy.
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- H. Y. McSween
- Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996–1410, USA.
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- M. T. Zuber
- Massachussetts Institute of Technology, Cambridge, MA 02139–4307, USA.
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- A. Nathues
- Max-Planck-Institut fur Sonnensystemforschung, Katlenburg-Lindau, Germany.
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- M. C. De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy.
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- R. Jaumann
- Institute of Planetary Research, DLR, Berlin, Germany.
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- A. S. Konopliv
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
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- F. Preusker
- Institute of Planetary Research, DLR, Berlin, Germany.
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- S. W. Asmar
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
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- R. S. Park
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
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- R. Gaskell
- Planetary Science Institute, Tucson, AZ 85719, USA.
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- H. U. Keller
- Max-Planck-Institut fur Sonnensystemforschung, Katlenburg-Lindau, Germany.
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- S. Mottola
- Institute of Planetary Research, DLR, Berlin, Germany.
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- T. Roatsch
- Institute of Planetary Research, DLR, Berlin, Germany.
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- J. E. C. Scully
- Department of Earth and Space Sciences, University of California, Los Angeles, CA 90095–1567, USA.
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- D. E. Smith
- Massachussetts Institute of Technology, Cambridge, MA 02139–4307, USA.
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- P. Tricarico
- Planetary Science Institute, Tucson, AZ 85719, USA.
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- M. J. Toplis
- Institut de Recherche en Astrophysique et Planetologie, Université de Toulouse, France.
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- U. R. Christensen
- Max-Planck-Institut fur Sonnensystemforschung, Katlenburg-Lindau, Germany.
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- W. C. Feldman
- Planetary Science Institute, Tucson, AZ 85719, USA.
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- D. J. Lawrence
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA.
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- T. J. McCoy
- Smithsonian Institution, Washington, DC 20560, USA.
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- T. H. Prettyman
- Planetary Science Institute, Tucson, AZ 85719, USA.
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- R. C. Reedy
- Planetary Science Institute, Tucson, AZ 85719, USA.
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- M. E. Sykes
- Planetary Science Institute, Tucson, AZ 85719, USA.
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- T. N. Titus
- U.S. Geological Survey, Flagstaff, AZ 86001, USA.
書誌事項
- 公開日
- 2012-05-11
- DOI
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- 10.1126/science.1219381
- 公開者
- American Association for the Advancement of Science (AAAS)
この論文をさがす
説明
<jats:title>A New Dawn</jats:title> <jats:p> Since 17 July 2011, NASA's spacecraft Dawn has been orbiting the asteroid Vesta—the second most massive and the third largest asteroid in the solar system (see the cover). <jats:bold> Russell <jats:italic>et al.</jats:italic> </jats:bold> (p. <jats:related-article xmlns:xlink="http://www.w3.org/1999/xlink" ext-link-type="doi" page="684" related-article-type="in-this-issue" vol="336" xlink:href="10.1126/science.1219381">684</jats:related-article> ) use Dawn's observations to confirm that Vesta is a small differentiated planetary body with an inner core, and represents a surviving proto-planet from the earliest epoch of solar system formation; Vesta is also confirmed as the source of the howardite-eucrite-diogenite (HED) meteorites. <jats:bold> Jaumann <jats:italic>et al.</jats:italic> </jats:bold> (p. <jats:related-article xmlns:xlink="http://www.w3.org/1999/xlink" ext-link-type="doi" page="687" related-article-type="in-this-issue" vol="336" xlink:href="10.1126/science.1219122">687</jats:related-article> ) report on the asteroid's overall geometry and topography, based on global surface mapping. Vesta's surface is dominated by numerous impact craters and large troughs around the equatorial region. <jats:bold> Marchi <jats:italic>et al.</jats:italic> </jats:bold> (p. <jats:related-article xmlns:xlink="http://www.w3.org/1999/xlink" ext-link-type="doi" page="690" related-article-type="in-this-issue" vol="336" xlink:href="10.1126/science.1218757">690</jats:related-article> ) report on Vesta's complex cratering history and constrain the age of some of its major regions based on crater counts. <jats:bold> Schenk <jats:italic>et al.</jats:italic> </jats:bold> (p. <jats:related-article xmlns:xlink="http://www.w3.org/1999/xlink" ext-link-type="doi" page="694" related-article-type="in-this-issue" vol="336" xlink:href="10.1126/science.1223272">694</jats:related-article> ) describe two giant impact basins located at the asteroid's south pole. Both basins are young and excavated enough amounts of material to form the Vestoids—a group of asteroids with a composition similar to that of Vesta—and HED meteorites. <jats:bold> De Sanctis <jats:italic>et al.</jats:italic> </jats:bold> (p. <jats:related-article xmlns:xlink="http://www.w3.org/1999/xlink" ext-link-type="doi" page="697" related-article-type="in-this-issue" vol="336" xlink:href="10.1126/science.1219270">697</jats:related-article> ) present the mineralogical characterization of Vesta, based on data obtained by Dawn's visual and infrared spectrometer, revealing that this asteroid underwent a complex magmatic evolution that led to a differentiated crust and mantle. The global color variations detailed by <jats:bold> Reddy <jats:italic>et al.</jats:italic> </jats:bold> (p. <jats:related-article xmlns:xlink="http://www.w3.org/1999/xlink" ext-link-type="doi" page="700" related-article-type="in-this-issue" vol="336" xlink:href="10.1126/science.1219088">700</jats:related-article> ) are unlike those of any other asteroid observed so far and are also indicative of a preserved, differentiated proto-planet. </jats:p>
収録刊行物
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- Science
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Science 336 (6082), 684-686, 2012-05-11
American Association for the Advancement of Science (AAAS)
