New Animation Takes a Colorful Flight Over Ceres 29 January 2016

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New animation takes a colorful flight over Ceres 29 January 2016 "The simulated overflight shows the wide range of crater shapes that we have encountered on Ceres. The viewer can observe the sheer walls of the crater Occator, and also Dantu and Yalode, where the craters are a lot flatter," said Ralf Jaumann, a Dawn mission scientist at DLR. Dawn is the first mission to visit Ceres, the largest object in the main asteroid belt between Mars and Jupiter. After orbiting asteroid Vesta for 14 months in 2011 and 2012, Dawn arrived at Ceres in March 2015. The spacecraft is currently in its final and lowest mapping orbit, at about 240 miles (385 Occator Crater (57 miles, 92 kilometers) on Ceres, home kilometers) from the surface. of the brightest spots on the dwarf planet, in a simulated view using Dawn images. Credit: NASA/JPL- Caltech/UCLA/MPS/DLR/IDA Provided by NASA A colorful new animation shows a simulated flight over the surface of dwarf planet Ceres, based on images from NASA's Dawn spacecraft. The movie shows Ceres in enhanced color, which helps to highlight subtle differences in the appearance of surface materials. Scientists believe areas with shades of blue contain younger, fresher material, including flows, pits and cracks. The animated flight over Ceres emphasizes the most prominent craters, such as Occator, and the tall, conical mountain Ahuna Mons. Features on Ceres are named for earthly agricultural spirits, deities and festivals. The movie was produced by members of Dawn's framing camera team at the German Aerospace Center, DLR, using images from Dawn's high- altitude mapping orbit. During that phase of the mission, which lasted from August to October 2015, the spacecraft circled Ceres at an altitude of about 900 miles (1,450 kilometers). 1 / 2 APA citation: New animation takes a colorful flight over Ceres (2016, January 29) retrieved 25 September 2021 from https://phys.org/news/2016-01-animation-flight-ceres.html This document is subject to copyright. Apart from any fair dealing for the purpose of private study or research, no part may be reproduced without the written permission. The content is provided for information purposes only. 2 / 2 Powered by TCPDF (www.tcpdf.org).

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The Puzzle of the Missing Large Craters. S
47th Lunar and Planetary Science Conference (2016) 1281.pdf CRATERING ON CERES: THE PUZZLE OF THE MISSING LARGE CRATERS. S. Marchi1, D. P. O'Brien2, P. Schenk3, R. Fu4, A. Ermakov5, M. C. De Sanctis6, E. Ammannito7, D. A. Williams8, S. C. Mest2, C. A. Raymond9, C. T. Russell7; 1Southwest Research Institute ([email protected]), Boulder, CO; 2Planetary Science Institute, Tucson, AZ; 3Lunar and Planetary Institute, Houston, TX; 4Lamont-Doherty Earth Ob- servatory, Palisades, NY; 5Massachusetts Institute of Technology, Cambridge, MA; 6Istituto Nazionale d'Astrofisica, Rome, Italy; 7University of California, Los Angeles, CA; 8Arizona State University, Tempe, AZ; 9JPL, Caltech, Pasadena, CA. Introduction: Data acquired by the Dawn space- hemisphere, although heavily craters terrains are also craft revealed a portrait of Ceres's surface that, in many found at low latitudes. This observation tells us that to- ways, challenges our preconceived expectations. pographic relaxation due to the presence of an ice-rich Ceres is the largest object in the main belt of aster- shell has to be limited. Furthermore, an improved oids. As such, extensive ground-based and Hubble model of topographic relaxation has constrained the Space Telescope observations have provided a wealth fraction of ice to be <30% in the outer shell [9]. of information [e.g. 1,2] Ceres' surface has a very low A second major finding is the lack of larger craters. albedo (~9 %) [2], while the lack of significant absorp- The largest well recognizable craters are 260-280 km tions bands at visible and near-infrared wavelengths in diameter. Although large scale topography relaxes points toward a more pristine composition [e.g., 3,4] if faster than at small scales, the lack of large craters compared to many siblings in the asteroid belt (and no- seems at odds with the presence of heavily cratered ter- tably to the large asteroid Vesta).
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1950 Da, 205, 269 1979 Va, 230 1991 Ry16, 183 1992 Kd, 61 1992
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