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Hestroffer D, Campo Bagatín A, Losert W, Opsomer E, Sánchez P, Scheeres DJ, Staron L, Taberlet N, Yano H, Eggl S, Lecomte CE, Murdoch N, Radjai F, Richardson DC, Salazar M, Schwartz SR, Tanga P. Small solar system bodies as granular systems. EPJ WEB OF CONFERENCES 2017. [DOI: 10.1051/epjconf/201714014011] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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González-Gutiérrez J, Carrillo-Estrada JL, Ruiz-Suárez JC. Penetration of granular projectiles into a water target. Sci Rep 2014; 4:6762. [PMID: 25342448 PMCID: PMC4208039 DOI: 10.1038/srep06762] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/11/2014] [Accepted: 10/06/2014] [Indexed: 11/09/2022] Open
Abstract
The penetration of low-speed projectiles into a water target has been studied in the last several years to understand the physics behind the formation and collapse of cavities. In such studies, the projectiles employed were solid bodies or liquid drops. Here we report similar impact experiments using granular projectiles, with the aim to investigate how the morphology of the cavities is determined by the balance between the dynamic pressure exerted by the fluid and the cohesive strength of the impactors. From the results we present and discuss in this manuscript, we speculate on the dynamics of meteorite disintegration in the atmosphere of our planet.
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Affiliation(s)
- Jorge González-Gutiérrez
- 1] Centro de Investigación y de Estudios Avanzados, Unidad Monterrey, PIIT Autopista al Aeropuerto Km. 9.5, Apodaca, Nuevo León 66600, México [2] Instituto de Física, Benemérita Universidad Autónoma de Puebla, A. P. J-48, Puebla 72570, México
| | - J L Carrillo-Estrada
- Instituto de Física, Benemérita Universidad Autónoma de Puebla, A. P. J-48, Puebla 72570, México
| | - J C Ruiz-Suárez
- Centro de Investigación y de Estudios Avanzados, Unidad Monterrey, PIIT Autopista al Aeropuerto Km. 9.5, Apodaca, Nuevo León 66600, México
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Ruiz-Suárez JC. Penetration of projectiles into granular targets. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2013; 76:066601. [PMID: 23660625 DOI: 10.1088/0034-4885/76/6/066601] [Citation(s) in RCA: 34] [Impact Index Per Article: 3.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
Energetic collisions of subatomic particles with fixed or moving targets have been very valuable to penetrate into the mysteries of nature. But the mysteries are quite intriguing when projectiles and targets are macroscopically immense. We know that countless debris wandering in space impacted (and still do) large asteroids, moons and planets; and that millions of craters on their surfaces are traces of such collisions. By classifying and studying the morphology of such craters, geologists and astrophysicists obtain important clues to understand the origin and evolution of the Solar System. This review surveys knowledge about crater phenomena in the planetary science context, avoiding detailed descriptions already found in excellent papers on the subject. Then, it examines the most important results reported in the literature related to impact and penetration phenomena in granular targets obtained by doing simple experiments. The main goal is to discern whether both schools, one that takes into account the right ingredients (planetary bodies and very high energies) but cannot physically reproduce the collisions, and the other that easily carries out the collisions but uses laboratory ingredients (small projectiles and low energies), can arrive at a synergistic intersection point.
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Fujiwara A, Kawaguchi J, Yeomans DK, Abe M, Mukai T, Okada T, Saito J, Yano H, Yoshikawa M, Scheeres DJ, Barnouin-Jha O, Cheng AF, Demura H, Gaskell RW, Hirata N, Ikeda H, Kominato T, Miyamoto H, Nakamura AM, Nakamura R, Sasaki S, Uesugi K. The rubble-pile asteroid Itokawa as observed by Hayabusa. Science 2006; 312:1330-4. [PMID: 16741107 DOI: 10.1126/science.1125841] [Citation(s) in RCA: 74] [Impact Index Per Article: 4.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
During the interval from September through early December 2005, the Hayabusa spacecraft was in close proximity to near-Earth asteroid 25143 Itokawa, and a variety of data were taken on its shape, mass, and surface topography as well as its mineralogic and elemental abundances. The asteroid's orthogonal axes are 535, 294, and 209 meters, the mass is 3.51 x 10(10) kilograms, and the estimated bulk density is 1.9 +/- 0.13 grams per cubic centimeter. The correspondence between the smooth areas on the surface (Muses Sea and Sagamihara) and the gravitationally low regions suggests mass movement and an effective resurfacing process by impact jolting. Itokawa is considered to be a rubble-pile body because of its low bulk density, high porosity, boulder-rich appearance, and shape. The existence of very large boulders and pillars suggests an early collisional breakup of a preexisting parent asteroid followed by a re-agglomeration into a rubble-pile object.
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Affiliation(s)
- A Fujiwara
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan.
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Dunham DW, Farquhar RW, McAdams JV. Recent gravity-assist trajectories for interplanetary and solar exploration. Ann N Y Acad Sci 2006; 1065:254-70. [PMID: 16510413 DOI: 10.1196/annals.1370.006] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
Abstract
This paper describes how lunar and planetary gravity assists have been used to design trajectories that have enabled challenging missions, currently flying or in development, at the Applied Physics Laboratory (APL) of Johns Hopkins University, to explore the Sun, and the planets closest to and farthest from it. This is a continuation of a paper presented at the first New Trends in Astrodynamics and Applications conference, January 2003. That paper concentrated on the Third International Sun-Earth Explorer (ISEE-3) halo orbit mission, later known as the International Cometary Explorer, or ICE, and the Near Earth Asteroid Rendezvous (NEAR) mission of APL, and the ground-breaking orbits that those spacecraft used to accomplish their ambitious goals. This paper gives much more information about current APL missions, MESSENGER, STEREO, and New Horizons, which were only briefly described in the previous paper.
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Affiliation(s)
- David W Dunham
- Applied Physics Laboratory, The Johns Hopkins University, 11100 Johns Hopkins Rd., Laurel, MD 20723-6099, USA.
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Thomas PC, Parker JW, McFadden LA, Russell CT, Stern SA, Sykes MV, Young EF. Differentiation of the asteroid Ceres as revealed by its shape. Nature 2005; 437:224-6. [PMID: 16148926 DOI: 10.1038/nature03938] [Citation(s) in RCA: 239] [Impact Index Per Article: 12.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/22/2005] [Accepted: 06/10/2005] [Indexed: 11/08/2022]
Abstract
The accretion of bodies in the asteroid belt was halted nearly 4.6 billion years ago by the gravitational influence of the newly formed giant planet Jupiter. The asteroid belt therefore preserves a record of both this earliest epoch of Solar System formation and variation of conditions within the solar nebula. Spectral features in reflected sunlight indicate that some asteroids have experienced sufficient thermal evolution to differentiate into layered structures. The second most massive asteroid--4 Vesta--has differentiated to a crust, mantle and core. 1 Ceres, the largest and most massive asteroid, has in contrast been presumed to be homogeneous, in part because of its low density, low albedo and relatively featureless visible reflectance spectrum, similar to carbonaceous meteorites that have suffered minimal thermal processing. Here we show that Ceres has a shape and smoothness indicative of a gravitationally relaxed object. Its shape is significantly less flattened than that expected for a homogeneous object, but is consistent with a central mass concentration indicative of differentiation. Possible interior configurations include water-ice-rich mantles over a rocky core.
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Affiliation(s)
- P C Thomas
- Center for Radiophysics and Space Research, Cornell University, Ithaca, New York 14853, USA.
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Dunham DW, Farquhar RW. Background and applications of astrodynamics for space missions of the johns hopkins applied physics laboratory. Ann N Y Acad Sci 2004; 1017:267-306. [PMID: 15220152 DOI: 10.1196/annals.1311.016] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
Abstract
This paper describes astrodynamic techniques applied to develop special orbital designs for past and future space missions of the Applied Physics Laboratory (APL) of Johns Hopkins University, and background about those techniques. The paper does not describe the long history of low Earth-orbiting missions at APL, but rather concentrates on the astrodynamically more interesting high-altitude and interplanetary missions that APL has undertaken in recent years. The authors developed many of their techniques in preparation for, and during, the Third International Sun-Earth Explorer (ISEE-3) halo orbit mission while they worked for the Goddard Space Flight Center (GSFC) of NASA during the 1970s and 1980s. Later missions owed much to the ground breaking work of the trajectory designs for ISEE-3 (later known as the International Cometary Explorer, or ICE). This experience, and other new ideas, were applied to the APL near Earth asteroid rendezvous (NEAR) and comet nucleus tour (CONTOUR) discovery missions, as well as to APL's future MESSENGER, STEREO, and New Horizons missions. These will be described in the paper.
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Affiliation(s)
- David W Dunham
- Applied Physics Laboratory, Johns Hopkins University, Baltimore, MA, USA.
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Soderblom LA, Becker TL, Bennett G, Boice DC, Britt DT, Brown RH, Buratti BJ, Isbell C, Giese B, Hare T, Hicks MD, Howington-Kraus E, Kirk RL, Lee M, Nelson RM, Oberst J, Owen TC, Rayman MD, Sandel BR, Stern SA, Thomas N, Yelle RV. Observations of comet 19P/Borrelly by the miniature integrated camera and spectrometer aboard Deep Space 1. Science 2002; 296:1087-91. [PMID: 11934989 DOI: 10.1126/science.1069527] [Citation(s) in RCA: 182] [Impact Index Per Article: 8.3] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The nucleus of the Jupiter-family comet 19P/Borrelly was closely observed by the Miniature Integrated Camera and Spectrometer aboard the Deep Space 1 spacecraft on 22 September 2001. The 8-kilometer-long body is highly variegated on a scale of 200 meters, exhibiting large albedo variations (0.01 to 0.03) and complex geologic relationships. Short-wavelength infrared spectra (1.3 to 2.6 micrometers) show a slope toward the red and a hot, dry surface (</=345 kelvin, with no trace of water ice or hydrated minerals), consistent with approximately 10% or less of the surface actively sublimating. Borrelly's coma exhibits two types of dust features: fans and highly collimated jets. At encounter, the near-nucleus coma was dominated by a prominent dust jet that resolved into at least three smaller jets emanating from a broad basin in the middle of the nucleus. Because the major dust jet remained fixed in orientation, it is evidently aligned near the rotation axis of the nucleus.
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Affiliation(s)
- L A Soderblom
- United States Geological Survey, 2255 North Gemini Drive, Flagstaff, AZ 86001, USA.
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Size-Frequency Distributions of Planetary Impact Craters and Asteroids. COLLISIONAL PROCESSES IN THE SOLAR SYSTEM 2001. [DOI: 10.1007/978-94-010-0712-2_1] [Citation(s) in RCA: 29] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 02/04/2023]
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Neukum G, Ivanov BA, Hartmann WK. Cratering Records in the Inner Solar System in Relation to the Lunar Reference System. SPACE SCIENCES SERIES OF ISSI 2001. [DOI: 10.1007/978-94-017-1035-0_3] [Citation(s) in RCA: 82] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/13/2022]
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Veverka J, Robinson M, Thomas P, Murchie S, Bell JF, Izenberg N, Chapman C, Harch A, Bell M, Carcich B, Cheng A, Clark B, Domingue D, Dunham D, Farquhar R, Gaffey MJ, Hawkins E, Joseph J, Kirk R, Li H, Lucey P, Malin M, Martin P, McFadden L, Merline WJ, Miller JK. NEAR at eros: imaging and spectral results. Science 2000; 289:2088-97. [PMID: 11000105 DOI: 10.1126/science.289.5487.2088] [Citation(s) in RCA: 200] [Impact Index Per Article: 8.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Eros is a very elongated (34 kilometers by 11 kilometers by 11 kilometers) asteroid, most of the surface of which is saturated with craters smaller than 1 kilometer in diameter. The largest crater is 5.5 kilometers across, but there is a 10-kilometer saddle-like depression with attributes of a large degraded crater. Surface lineations, both grooves and ridges, are prominent on Eros; some probably exploit planes of weakness produced by collisions on Eros and/or its parent body. Ejecta blocks (30 to 100 meters across) are abundant but not uniformly distributed over the surface. Albedo variations are restricted to the inner walls of certain craters and may be related to downslope movement of regolith. On scales of 200 meters to 1 kilometer, Eros is more bland in terms of color variations than Gaspra or Ida. Spectra (800 to 2500 nanometers) are consistent with an ordinary chondrite composition for which the measured mean density of 2.67 +/- 0.1 grams per cubic centimeter implies internal porosities ranging from about 10 to 30 percent.
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Affiliation(s)
- J Veverka
- Space Sciences Building, Cornell University, Ithaca, NY 14853, USA. Department of Geological Sciences, Northwestern University, 309 Locy Hall, Evanston, IL 60208, USA. Applied Physics Laboratory, Johns Hopkins University, 1110 Johns Hopkins Road, L
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Housen KR, Holsapple KA, Voss ME. Compaction as the origin of the unusual craters on the asteroid Mathilde. Nature 1999. [DOI: 10.1038/45985] [Citation(s) in RCA: 83] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/16/2022]
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Merline WJ, Close LM, Dumas C, Chapman CR, Roddier F, Ménard F, Slater DC, Duvert G, Shelton C, Morgan T. Discovery of a moon orbiting the asteroid 45 Eugenia. Nature 1999. [DOI: 10.1038/44089] [Citation(s) in RCA: 76] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Clark BC, Baker AL, Cheng AF, Clemett SJ, McKay D, McSween HY, Pieters CM, Thomas P, Zolensky M. Survival of life on asteroids, comets and other small bodies. ORIGINS LIFE EVOL B 1999; 29:521-45. [PMID: 10573692 DOI: 10.1023/a:1006589213075] [Citation(s) in RCA: 24] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
Abstract
The ability of living organisms to survive on the smaller bodies in our solar system is examined. The three most significant sterilizing effects include ionizing radiation, prolonged extreme vacuum, and relentless thermal inactivation. Each could be effectively lethal, and even more so in combination, if organisms at some time resided in the surfaces of airless small bodies located near or in the inner solar system. Deep within volatile-rich bodies, certain environments theoretically might provide protection of dormant organisms against these sterilizing factors. Sterility of surface materials to tens or hundreds of centimeters of depth appears inevitable, and to greater depths for bodies which have resided for long periods sunward of about 2 A.U.
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Affiliation(s)
- B C Clark
- Advanced Planetary Studies Group, Lockheed Martin Astronautics, Denver, CO, USA
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Ostro SJ, Pravec P, Benner LA, Hudson RS, Sarounova L, Hicks MD, Rabinowitz DL, Scotti JV, Tholen DJ, Wolf M, Jurgens RF, Thomas ML, Giorgini JD, Chodas PW, Yeomans DK, Rose R, Frye R, Rosema KD, Winkler R, Slade MA. Radar and optical observations of asteroid 1998 KY26. Science 1999; 285:557-60. [PMID: 10417379 DOI: 10.1126/science.285.5427.557] [Citation(s) in RCA: 41] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Observations of near-Earth asteroid 1998 KY26 shortly after its discovery reveal a slightly elongated spheroid with a diameter of about 30 meters, a composition analogous to carbonaceous chondritic meteorites, and a rotation period of 10.7 minutes, which is an order of magnitude shorter than that measured for any other solar system object. The rotation is too rapid for 1998 KY26 to consist of multiple components bound together just by their mutual gravitational attraction. This monolithic object probably is a fragment derived from cratering or collisional destruction of a much larger asteroid.
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Affiliation(s)
- SJ Ostro
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA. Astronomical Institute, Academy of Sciences of the Czech Republic, CZ-25165 Ond&rbreve;ejov, Czech Republic. School of Electrical Engineering and
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Veverka J, Thomas PC, Bell JF, Bell M, Carcich B, Clark B, Harch A, Joseph J, Martin P, Robinson M, Murchie S, Izenberg N, Hawkins E, Warren J, Farquhar R, Cheng A, Dunham D, Chapman C, Merline WJ, McFadden L, Wellnitz D, Malin M, Owen WM, Miller JK, Williams BG, Yeomans DK. Imaging of asteroid 433 eros during NEAR's flyby reconnaissance. Science 1999; 285:562-4. [PMID: 10417381 DOI: 10.1126/science.285.5427.562] [Citation(s) in RCA: 43] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/03/2022]
Abstract
During the 23 December 1998 flyby of asteroid 433 Eros, the Near-Earth Asteroid Rendezvous (NEAR) spacecraft obtained 222 images of Eros, as well as supporting spectral observations. The images cover slightly more than two-thirds of Eros (best resolution is approximately 400 meters per pixel) and reveal an elongated, cratered body with a linear feature extending for at least 20 kilometers. Our observations show that Eros has dimensions of 33 x 13 x 13 kilometers. The volume, combined with the mass determined by the NEAR radio science experiment, leads to a density of 2.5 +/- 0.8 grams per cubic centimeter. This relatively high density, and the presence of an extensive linear feature, suggest that Eros may be a structurally coherent body.
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Affiliation(s)
- J Veverka
- Space Sciences Building, Cornell University, Ithaca, NY 14853, USA. Department of Geological Sciences, Northwestern University, 309 Locy Hall, Evanston, IL 60208, USA. Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA. Sou
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Asphaug E, Ostro SJ, Hudson RS, Scheeres DJ, Benz W. Disruption of kilometre-sized asteroids by energetic collisions. Nature 1998. [DOI: 10.1038/30911] [Citation(s) in RCA: 132] [Impact Index Per Article: 5.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Affiliation(s)
- Erik Asphaug
- The author is at the SETI Institute/NASA, Ames Research Center, Moffett Field, CA 94305, USA
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Yeomans DK, Barriot J, Dunham DW, Farquhar RW, Giorgini JD, Helfrich CE, Konopliv AS, McAdams JV, Miller JK, Owen WM, Scheeres DJ, Synnott SP, Williams BG. Estimating the mass of asteroid 253 mathilde from tracking data during the NEAR flyby. Science 1997; 278:2106-9. [PMID: 9405343 DOI: 10.1126/science.278.5346.2106] [Citation(s) in RCA: 146] [Impact Index Per Article: 5.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/05/2023]
Abstract
The terminal navigation of the Near Earth Asteroid Rendezvous (NEAR) spacecraft during its close flyby of asteroid 253 Mathilde involved coordinated efforts to determine the heliocentric orbits of the spacecraft and Mathilde and then to determine the relative trajectory of the spacecraft with respect to Mathilde. The gravitational perturbation of Mathilde on the passing spacecraft was apparent in the spacecraft tracking data. As a result of the accurate targeting achieved, these data could be used to determine Mathilde's mass as 1.033 (+/- 0.044) x 10(20) grams. Coupled with a volume estimate provided by the NEAR imaging team, this mass suggests a low bulk density for Mathilde of 1.3 grams per cubic centimeter.
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Affiliation(s)
- DK Yeomans
- D. K. Yeomans, J. D. Giorgini, C. E. Helfrich, A. S. Konopliv, J. K. Miller, W. M. Owen Jr., D. J. Scheeres, S. P. Synnott, B. G. Williams, Navigation and Flight Mechanics Section, Jet Propulsion Laboratory (JPL), California Institute of Tech
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