Differentiation of the asteroid Ceres as revealed by its shape
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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Ceres is likely differentiated into a rocky core and icy shell.
“It is 25% the size of our Moon and twice the size of Enceladus and likely differentiated into a rocky core and icy shell (McCord and Sotin, 2005; Thomas et al., 2005).”
From The Astrobiology Primer v2.0 (2016) · cites this paper as Thomas et al., 2005
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“explained with a significant ice mantle (Thomas et al. 2005).”
BackgroundPerryman, M. A. C. (2018) · Cambridge University Press eBooks · doi:10.1017/9781108304160.017 · Cited by 89 · see citing works
Ciarniello, M., Sanctis, M. C. D., Ammannito, E., et al. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201629490 · Cited by 84 · see citing works
“Interior models based on shape data indicated that Ceres is a gravitationally relaxed and likely differentiated object (Thomas et al. 2005; Castillo-Rogez & McCord 2010) with a rocky core and a hydrated (icy or liquid) mantle (Neveu et al. 2015; Neveu & Desch 2015).”
MethodSelf-citationResolved spectrophotometric properties of the Ceres surface from Dawn Framing Camera images
Schröder, S. E., Mottola, S., Carsenty, U., Ciarniello, M., Jaumann, R., Li, J., Longobardo, A., Palmer, E. E., Pieters, C. M., Preusker, F., et al. (2017) · Icarus · doi:10.1016/j.icarus.2017.01.026 · Cited by 83 · see citing works
Self-citationThe Dawn Gravity Investigation at Vesta and Ceres
Konopliv, A. S., Asmar, S. W., Bills, B. G., Mastrodemos, N., Park, R. S., Raymond, C. A., Smith, D. E., & Zuber, M. T. (2011) · Space Science Reviews · doi:10.1007/s11214-011-9794-8 · Cited by 84 · see citing works
Konopliv, A. S., Park, R. S., Vaughan, A. T., et al. (2017) · Icarus · doi:10.1016/j.icarus.2017.08.005 · Cited by 83 · see citing works
Self-citationMain belt binary asteroidal systems with eccentric mutual orbits
Marchis, F., Descamps, P., Berthier, J., et al. (2008) · Icarus · doi:10.1016/j.icarus.2007.12.010 · Cited by 81 · see citing works
“This density measurement is very close to the bulk density of (1) Ceres, another G-type asteroid, which was inferred by Thomas et al. (2005) from the ellipsoidal shape of this large asteroid.”
MethodThermal and Compositional Evolution of the Core
Nimmo, F. (2015) · Elsevier eBooks · doi:10.1016/b978-0-444-53802-4.00160-3 · Cited by 81 · see citing works
THE SURVIVAL OF WATER WITHIN EXTRASOLAR MINOR PLANETS
Jura, M., & Xu, S.-Y. (2010) · The Astronomical Journal · doi:10.1088/0004-6256/140/5/1129 · Cited by 57 · see citing works
“For example, in the Solar System, Ceres, the most massive asteroid, has a mean density of 2.1 g cm−3 suggesting ∼25% of its mass is water (McCord & Sotin 2005, Thomas et al. 2005).”
BackgroundInfluentialThe Origin and Evolution of the Asteroid Belt—Implications for Vesta and Ceres
O'Brien, D. P., & Sykes, M. V. (2011) · Space Science Reviews · doi:10.1007/s11214-011-9808-6 · Cited by 78 · see citing works
Self-citationPercolative core formation in planetesimals
Terasaki, H., Frost, D. J., Rubie, D. C., et al. (2008) · Earth and Planetary Science Letters · doi:10.1016/j.epsl.2008.06.019 · Cited by 76 · see citing works
Physical properties of (2) Pallas
Carry, B., Dumas, C., Kaasalainen, M., et al. (2009) · Icarus · doi:10.1016/j.icarus.2009.08.007 · Cited by 75 · see citing works
“The deconvolution process is an ill-posed inverse problem (Tikhonov and Arsenine, 1974) and can introduce artifacts in the restored images.”
BackgroundAstrometric masses of 21 asteroids, and an integrated asteroid ephemeris
Baer, J., & Chesley, S. R. (2007) · Celestial Mechanics and Dynamical Astronomy · doi:10.1007/s10569-007-9103-8 · Cited by 72 · see citing works
“3.58±0.42×10−11 4.29 ± 1.39 804 1002 4.69±1.85 ×10−12 2.5 4.55 ± 2.27 P 158 × 158 × 158e 8e References:a Thomas et al. (2005); b Dunham et al. (1990); c Thomas et al. (1997); d Torppa et al. (2003); e Tedesco et al. (2002); f Kaasalainen et al. (2002); g Kissling et al. (1991); h Storrs et al.…”
InfluentialTaubner, R.-S., Schleper, C., Firneis, M. G., & Rittmann, S. K. ‐. R. (2015) · Life · doi:10.3390/life5041652 · Cited by 72 · see citing works
Exposed H2O-rich areas detected on Ceres with the dawn visible and infrared mapping spectrometer
Combe, J., Raponi, A., Tosi, F., et al. (2017) · Icarus · doi:10.1016/j.icarus.2017.12.008 · Cited by 71 · see citing works
Self-citationShape modeling technique KOALA validated by ESA Rosetta at (21) Lutetia
Carry, B., Kaasalainen, M., Merline, W. J., et al. (2011) · Planetary and Space Science · doi:10.1016/j.pss.2011.12.018 · Cited by 66 · see citing works
A water–ice rich minor body from the early Solar System: The CR chondrite parent asteroid
Schrader, D. L., Davidson, J., Greenwood, R. C., Franchi, I. A., & Gibson, J. M. (2014) · Earth and Planetary Science Letters · doi:10.1016/j.epsl.2014.09.030 · Cited by 66 · see citing works
Rubie, D. C., Nimmo, F., & Melosh, H. J. (2015) · Elsevier eBooks · doi:10.1016/b978-0-444-53802-4.00154-8 · Cited by 66 · see citing works
Infrared Emission from the Dusty Disk Orbiting GD 362, An Externally-Polluted White DwarfPreprint
Jura, M., Farihi, J., Zuckerman, B., et al. (2007) · Cited by 65 · see citing works
Odert, P., Lammer, H., Erkaev, N. V., Nikolaou, A., Lichtenegger, H., Johnstone, C. P., Kislyakova, K. G., Leitzinger, M., & Tosi, N. (2017) · Icarus · doi:10.1016/j.icarus.2017.10.031 · Cited by 65 · see citing works
On the origin and composition of Theia: Constraints from new models of the Giant Impact
MEIER, M. M. M., Reufer, A., & WIELER, R. (2014) · Icarus · doi:10.1016/j.icarus.2014.08.003 · Cited by 63 · see citing works
The vanishing cryovolcanoes of Ceres
Sori, M. M., Byrne, S., Bland, M. T., et al. (2017) · Geophysical Research Letters · doi:10.1002/2016gl072319 · Cited by 63 · see citing works
Self-citationAqueous origins of bright salt deposits on Ceres
Zolotov, M. Y. (2017) · Icarus · doi:10.1016/j.icarus.2017.06.018 · Cited by 61 · see citing works
Ceres: Astrobiological Target and Possible Ocean World
Castillo-Rogez, J. C., Neveu, M. F., Scully, J. E. C., House, C. H., Quick, L. C., Bouquet, A., Miller, K. E., Bland, M. T., Sanctis, M. C. D., Ermakov, A., et al. (2020) · Astrobiology · doi:10.1089/ast.2018.1999 · Cited by 61 · see citing works
“However, thermal evolution models of Ceres, using shape data derived from telescopic observations ( e.g. , Thomas et al. , 2005; Carry et al. , 2008; Drummond et al. , 2014), indicate that, following accretion, the dwarf planet could have differentiated into a silicate core and a water-rich outer…”
Self-citationA frequency comb calibrated solar atlas
Molaro, P., Esposito, M., Monai, S., Curto, G. L., Hernández, J. I. G., Hänsch, T., Holzwarth, R., Manescau, A., Pasquini, L., Probst, R., et al. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201322324 · Cited by 49 · see citing works
Perryman, M. A. C. (2011) · Cambridge University Press eBooks · doi:10.1017/cbo9780511994852.011 · Cited by 71 · see citing works
Predicted crater morphologies on Ceres: Probing internal structure and evolution
Bland, M. T. (2013) · Icarus · doi:10.1016/j.icarus.2013.05.037 · Cited by 58 · see citing works
“The basic morphology (i.e., relaxation state) of Ceres’ craters alone can constrain whether the expected thick ice layer (e.g., McCord and Sotin, 2005; Thomas et al., 2005; Castillo-Rogez and McCord, 2010, and many others) actually exists in Ceres’ near-surface.”
InfluentialFormation of brucite and cronstedtite-bearing mineral assemblages on Ceres
Zolotov, M. Y. (2013) · Icarus · doi:10.1016/j.icarus.2013.09.020 · Cited by 57 · see citing works
“The polar flattening determined with Hubble Space Telescope is consistent with a relaxed differentiated body with a rocky core and an icy mantle (Thomas et al., 2005; Castillo-Rogez and McCord, 2010), though such an internal structure awaits verification.”
BackgroundPost-impact thermal structure and cooling timescales of Occator crater on asteroid 1 Ceres
Bowling, T. J., Ciesla, F. J., Davison, T. M., et al. (2018) · Icarus · doi:10.1016/j.icarus.2018.08.028 · Cited by 57 · see citing works
“…the arrival of Dawn, with several pre-encounter detections of water outgassing from the dwarf planet (A’Hearn and Feldman, 1992; Kuppers et al, 2014), constraints on the mass fraction of volatiles within the body could only be loosely inferred from the geodetic constraints (Thomas et al., 2005).”
BackgroundPossible signs of water and differentiation in a rocky exoplanetary body
Farihi, J., Brinkworth, C., Gänsicke, B., Marsh, T., Girven, J., Hoard, D., Klein, B., & Koester, D. (2011) · UCL Discovery (University College London) · Cited by 57 · see citing works
WATER FRACTIONS IN EXTRASOLAR PLANETESIMALSPreprint
Jura, M. A., & Xu, S. (2016) · Cited by 57 · see citing works
Instrumental methods for professional and amateur collaborations in planetary astronomy
Mousis, O. J., Hueso, R., Beaulieu, J., Bouley, S., Carry, B., Colas, F., Klotz, A., Pellier, C., Petit, J.-M., Rousselot, P., et al. (2014) · Experimental Astronomy · doi:10.1007/s10686-014-9379-0 · Cited by 56 · see citing works
“The amateur contribution to the study of this vortex has been extensive, including its long-term history and length variations (roughly from 40,000 km at the end of the 19th century to 20,000 km at present), its 90-day zonal oscillation [195], and its rare interactions with smaller ovals [163], examples of which led t…”
BackgroundSURFACE ALBEDO AND SPECTRAL VARIABILITY OF CERES
Li, J., Reddy, V., Nathues, A., Corre, L. L., Izawa, M. R. M., Cloutis, E. A., Sykes, M. V., Carsenty, U., Castillo-Rogez, J. C., Hoffmann, M., et al. (2016) · The Astrophysical Journal Letters · doi:10.3847/2041-8205/817/2/l22 · Cited by 54 · see citing works
“Note that Haulani crater is in fact the brightest feature on Ceres in HST images (Li et al. 2006, Thomas et al. 2005), brighter than Occator crater (Fig.”
BackgroundSelf-citationCryogenic flow features on Ceres: Implications for crater‐related cryovolcanism
Krohn, K., Jaumann, R., Stephan, K., et al. (2016) · Geophysical Research Letters · doi:10.1002/2016gl070370 · Cited by 54 · see citing works
“The potential presence of ice within Ceresˈ crust [McCord and Sotin, 2005] raises the prospect of geological processes similar to those on differentiated icy bodies [Thomas et al., 2005].”
BackgroundSelf-citationCeres: Its Origin, Evolution and Structure and Dawn’s Potential Contribution
McCord, T. B., Castillo-Rogez, J. C., & Rivkin, A. S. (2011) · Space Science Reviews · doi:10.1007/s11214-010-9729-9 · Cited by 54 · see citing works
New Constraints on the Abundance and Composition of Organic Matter on Ceres
Kaplan, H. H., Milliken, R. E., & Alexander, C. M. O. (2018) · Geophysical Research Letters · doi:10.1029/2018gl077913 · Cited by 54 · see citing works
“5278 mean-square error) of the spectral model are achieved with the highest H/C kerogen, an H/C value that would be indicative of minimal thermal alteration for Ceres as proposed previously (e.g., McCord & Sotin, 2005; Thomas et al., 2005).”
MethodDrummond, J., & Christou, J. C. (2008) · Icarus · doi:10.1016/j.icarus.2008.05.009 · Cited by 54 · see citing works
Core cracking and hydrothermal circulation can profoundly affect Ceres' geophysical evolution
Neveu, M. F., Desch, S. J., & Castillo-Rogez, J. C. (2014) · Journal of Geophysical Research Planets · doi:10.1002/2014je004714 · Cited by 53 · see citing works
The Dawn Topography Investigation
Raymond, C. A., Jaumann, R., Nathues, A., et al. (2011) · Space Science Reviews · doi:10.1007/s11214-011-9863-z · Cited by 53 · see citing works
“For Ceres, fewer data exist, but analysis of limb images by Thomas et al. (2005) has revealed the two axial diameters of Ceres to be 909 (polar) and 975 km (equatorial), whereas near-infrared imaging yields an estimate of a = b = 479 .”
InfluentialCeres – Neither a porous nor salty ball
Castillo-Rogez, J. C. (2011) · Icarus · doi:10.1016/j.icarus.2011.08.007 · Cited by 52 · see citing works
Ceres lightcurve analysis—Period determination
Chamberlain, M. A., Sykes, M. V., & Esquerdo, G. A. (2007) · Icarus · doi:10.1016/j.icarus.2006.11.025 · Cited by 52 · see citing works
Self-citationStructure and Evolution of Kuiper Belt Objects and Dwarf Planets
McKinnon, W. B., Prialnik, D., Stern, S. A., & Coradini, A. (2008) · Cited by 54 · see citing works
Self-citationWoodbury, D. P., & Junkins, J. L. (2010) · AIAA Guidance, Navigation, and Control Conference and Exhibit · doi:10.2514/6.2010-7752 · Cited by 51 · see citing works
Aléon, J., Engrand, C., Leshin, L. A., & McKeegan, K. D. (2009) · Geochimica et Cosmochimica Acta · doi:10.1016/j.gca.2009.04.034 · Cited by 50 · see citing works
Vesta and Ceres: Crossing the History of the Solar System
Coradini, A., Turrini, D., Federico, C., & Magni, G. (2011) · Space Science Reviews · doi:10.1007/s11214-011-9792-x · Cited by 50 · see citing works
“Thermal models of Ceres are mainly constrained by the gravitationally relaxed shape of the dwarf planet (Thomas et al. 2005).”
BackgroundThe impact crater at the origin of the Julia family detected with VLT/SPHERE?
Vernazza, P., Brož, M., Drouard, A., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201833477 · Cited by 48 · see citing works
Which are the dwarfs in the Solar System?
Tancredi, G., & Favre, S. (2008) · Icarus · doi:10.1016/j.icarus.2007.12.020 · Cited by 48 · see citing works
- Authors
- Thomas, P. C., Parker, J. W., McFadden, L. A., Russell, C. T., Stern, S. A., Sykes, M. V., & Young, E. F.
- Affiliations
- Cornell University (US)
- Southwest Research Institute (US)
- University of Maryland, College Park (US)
- University of California, Los Angeles (US)
- Planetary Science Institute (US)
- Corresponding author
- Thomas, P. C.
- Venue
- Nature
- Published
- 2005-09
- Volume
- 437
- Issue
- 7056
- Pages
- 224-226
- ISSN
- 0028-0836 (ISSN-L)
- 1476-4687
- OpenAlex
- W2055124830
- Semantic Scholar
- a23b0c9794d5736532a9b5148497f49fe879ad8e
- Cited by
- 303
- References
- 31
- Citations by year
- 2026: 4 · 2025: 3 · 2024: 6 · 2023: 4 · 2022: 11 · 2021: 8 · 2020: 5 · 2019: 8 · 2018: 37 · 2017: 25 · 2016: 23 · 2015: 22 · 2014: 22 · 2013: 13 · 2012: 5
- FWCI
- 6.79
- Type
- journal article
- Language
- en
- Open access
- closed
- Licence
- www.springer.com/tdm (tdm)
- Locations
- Nature (publishedVersion)
- PubMed (publishedVersion)
- RePEc: Research Papers in Economics (submittedVersion)
- Funders
- National Aeronautics and Space Administration
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Planetary Science and Exploration
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Keywords
- Ceres, asteroid shape, asteroid differentiation, gravitational relaxation, central mass concentration, ice mantles, rocky core, asteroid belt formation, solar nebula, thermal evolution, Vesta, asteroid albedo
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