The DOI matches its Crossref record; 31 of the 31 references it cites were found in a registry or an index.
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.
Overview
Integrity signals
Registry
Cites
Statistics
Verification
Claims the paper makes
Claims other papers make about this one
Each is checked against this paper’s own text: does it say what the citing paper says it does?
In the citing paper
“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
Citations
Cites
Impact cratering—A geologic process
LIPSCHUTZ, M. E. (1989) · Geochimica et Cosmochimica Acta · doi:10.1016/0016-7037(89)90150-6 · Cited by 2,279
Impact Cratering: A Geologic Process
Melosh, H. J. (1986) · Medical Entomology and Zoology · Cited by 2,077
Ellipsoidal Figures of Equilibrium
Chandrasekhar, S. (1969) · International Linear Collider · Cited by 1,439
Asteroid Vesta: Spectral Reflectivity and Compositional Implications
McCord, T. B., Adams, J. B., & Johnson, T. V. (1970) · Science · doi:10.1126/science.168.3938.1445 · Cited by 759
Stony meteorite porosities and densities: A review of the data through 2001
Britt, D. T., & Consolmagno, G. J. (2003) · Meteoritics and Planetary Science · doi:10.1111/j.1945-5100.2003.tb00305.x · Cited by 368
Water and the thermal evolution of carbonaceous chondrite parent bodies
Grimm, R. E., & McSWEEN, H. Y., Jr. (1989) · Icarus · doi:10.1016/0019-1035(89)90038-9 · Cited by 337
Impact Excavation on Asteroid 4 Vesta: Hubble Space Telescope Results
Thomas, P. C., Binzel, R. P., Gaffey, M. J., et al. (1997) · Science · doi:10.1126/science.277.5331.1492 · Cited by 315
Self-citationCeres: Evolution and current state
McCord, T. B., & Sotin, C. (2005) · Journal of Geophysical Research: Planets · doi:10.1029/2004je002244 · Cited by 272
A Thermal Model for the Differentiation of Asteroid 4 Vesta, Based on Radiogenic Heating
Ghosh, A., & McSWEEN, H. Y., Jr. (1998) · Icarus · doi:10.1006/icar.1998.5956 · Cited by 233
NEAR's Flyby of 253 Mathilde: Images of a C Asteroid
Veverka, J. F., Thomas, P. C., Harch, A. P., et al. (1997) · Science · doi:10.1126/science.278.5346.2109 · Cited by 204
Self-citation
Flagged first, then by citations
Research works printed but not linked: 2
- Rivkin, A. S. Observations of Main-belt Asteroids in the 3-µm Region. Ph.D. dissertation, Univ. Arizona (1997)
- Pavlovsky, C. et al. ACS Instrument Handbook, Version 5.0 (Space Telescope Science Institute, Baltimore, 2004)
Cited by
Sorted by citations
Items 101–200 of 303
Asteroid Models from Multiple Data Sources
Ďurech, J., Carry, B., Delbò, M., et al. (2015) · University of Arizona Press eBooks · doi:10.2458/azu_uapress_9780816532131-ch010 · Cited by 48
“olution and only the largest asteroids (1) Ceres, (2) Pallas, and (4) Vesta have been imaged. In the decade since Asteroids III, numerous studies have been based on direct imaging of asteroids (e.g., Thomas et al., 2005; Carry et al., 2008; Descamps et al., 2008; Schmidt et al., 2009; Marchis et al., 2013). Both from…”
BackgroundCometary masses derived from non-gravitational forces
Sosa, A., & Fernández, J. A. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.14183.x · Cited by 48
Sanctis, M. C. D., Ammannito, E., Carrozzo, F. G., Ciarniello, M., Giardino, M., Frigeri, A., Fonte, S., McSWEEN, H. Y., Jr., Raponi, A., Tosi, F., et al. (2018) · Meteoritics and Planetary Science · doi:10.1111/maps.13104 · Cited by 46
“Disk-resolved imaging of Ceres has allowed determination of its size, shape, spin, and density (Thomas et al. 2005; Carry et al. 2008).”
BackgroundSelf-citationThe case of the missing Ceres family
Rivkin, A. S., Asphaug, E. I., & Bottke, W. F. (2014) · Icarus · doi:10.1016/j.icarus.2014.08.007 · Cited by 43
Ceres: Its Origin, Evolution and Structure and Dawn’s Potential Contribution
McCord, T. B., Castillo-Rogez, J. C., & Rivkin, A. S. (2011) · Springer eBooks · doi:10.1007/978-1-4614-4903-4_5 · Cited by 43
Planetesimals to brown dwarfs: What is a planet?
Basri, G., & Brown, M. E. (2006) · Annual Review of Earth and Planetary Sciences · doi:10.1146/annurev.earth.34.031405.125058 · Cited by 52
“Empirically, however, it is easy to determine the largest bodies in the Solar System that have not cleared their region: Ceres is still surrounded by the asteroid belt, and Pluto and 2003 UB313 are still surrounded by the Kuiper belt.”
BackgroundInfluentialProbing the history of Solar system through the cratering records on Vesta and Ceres
Turrini, D., Magni, G., & Coradini, A. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.18316.x · Cited by 42
The Size and Shape of the Oblong Dwarf Planet Haumea
Lockwood, A. C., Brown, M. E., & Stansberry, J. (2014) · Earth Moon and Planets · doi:10.1007/s11038-014-9430-1 · Cited by 41
“…the size at which this rounding occurs in the outer solar system is not well known, the asteroid Ceres, with a diameter of 900 km is essentially round (Millis et al. 1987; Thomas et al. 2005), while among the icy satellites, everything the size of Mimas and larger (∼400 km) is essentially round.”
BackgroundCellino, A., Hestroffer, D., Tanga, P., et al. (2009) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200912134 · Cited by 41
“Again, we have to conclude that in the case of Ceres, as in the previously discussed case of Vesta, the photometric modulation displayed by the object must be caused mostly by albedo variegation of the surface, since the shape signature is very small.”
MethodResultInfluentialCeres water regime: surface temperature, water sublimation and transient exo(atmo)sphere
Formisano, M., Sanctis, M. D. D., Magni, G., Federico, C., & Capria, M. T. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2344 · Cited by 40
The Shape and Surface Variation of 2 Pallas from the Hubble Space Telescope
Schmidt, B. E., Thomas, P. C., Bauer, J. M., et al. (2009) · Science · doi:10.1126/science.1177734 · Cited by 41
Self-citationConstraining Ceres’ interior from its rotational motion
Rambaux, N., Castillo-Rogez, J., Dehant, V., et al. (2011) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201116563 · Cited by 40
“However, it has proved difficult to track surface landmarks with enough accuracy to constrain the polar orientation and rotation of the asteroid (Thomas et al. 2005; Carry et al. 2008; Drummond and Christou 2008).”
BackgroundMethodInfluentialVLT/SPHERE- and ALMA-based shape reconstruction of asteroid (3) Juno
Viikinkoski, M., Kaasalainen, M., Ďurech, J., et al. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201526626 · Cited by 39
“…(1) Ceres, (2) Pallas, and (4) Vesta witnessed by the Dawn mission (Russell et al. 2012) or imaged from the ground and Hubble Space Telescope (Thomas et al. 2005; Carry et al. 2008, 2010a), but typical of large asteroids that present large flat facets or concavities as do (21) Lutetia, (52)…”
Ceres's obliquity history and its implications for the permanently shadowed regions
Ermakov, A., Mazarico, E., Schröder, S. E., Carsenty, U., Schörghofer, N., Preusker, F., Raymond, C. A., Russell, C. T., & Zuber, M. T. (2017) · Geophysical Research Letters · doi:10.1002/2016gl072250 · Cited by 39
“The shape of dwarf planet (1) Ceres and orientation of its spin pole (and, therefore, obliquity) had been constrained in several studies prior to the Dawn mission [Thomas et al., 2005; Drummond and Christou, 2008; Carry et al., 2008; Drummond et al., 2014].”
BackgroundSelf-citationThe composition and structure of Ceres' interior
Zolotov, M. Y. (2019) · Icarus · doi:10.1016/j.icarus.2019.113404 · Cited by 42
Relationship between regolith particle size and porosity on small bodies
Kiuchi, M., & Nakamura, A. (2014) · Icarus · doi:10.1016/j.icarus.2014.05.029 · Cited by 38
Burbine, T. H. (2013) · Elsevier eBooks · doi:10.1016/b978-0-08-095975-7.00129-7 · Cited by 39
Herschel celestial calibration sources
Muller, T. G., Balog, Z., Nielbock, M., et al. (2013) · Experimental Astronomy · doi:10.1007/s10686-013-9357-y · Cited by 37
“argest and most massive asteroid in the main-belt. It is presumed to be homogeneous,gravitationally relaxed and it has a low density, low albedo and relatively featureless visible reflectance spectrum [78]. The shape that best reproduces the available data (occultations, HST measurements, adaptive optics studies, light…”
BackgroundMeteorites from the Outer Solar System
Gounelle, M., Morbidelli, A., Bland, P. A., Spurný, P., Young, E., & Sephton, M. A. (2008) · Cited by 36
Self-citationTricarico, P. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/782/2/99 · Cited by 36
“Its low density and fast rotation cause a significant polar flattening, consistent with the shape of an oblate spheroid, as determined by stellar occultation (Millis et al. 1987), HST observations (Thomas et al. 2005), and Keck AO observations (Carry et al. 2008).”
BackgroundMethodResultInfluentialPasckert, J. H., Hiesinger, H., Ruesch, O., et al. (2017) · Icarus · doi:10.1016/j.icarus.2017.06.015 · Cited by 35
Self-citationEvidence for the Interior Evolution of Ceres from Geologic Analysis of Fractures
Scully, J. E. C., Buczkowski, D. L., Schmedemann, N., et al. (2017) · Geophysical Research Letters · doi:10.1002/2017gl075086 · Cited by 35
Self-citationMASS DETERMINATION STUDIES OF 104 LARGE ASTEROIDS
Zielenbach, W. (2011) · The Astronomical Journal · doi:10.1088/0004-6256/142/4/120 · Cited by 35
“(1) Neese 2010; (2) Thomas et al. 2005; (3) Dunham et al. 1990; (4) Millis et al. 1981; (5) Kaasalainen et al. 2002; (6) Thomas et al. 1997; (7) JPL Small Bodies Database, http://ssd.jpl.nasa.gov/sbdb.cgi (enter the asteroid number under Search:); (8) Tedesco et al. 2002; (9) Torppa et al. 2003;…”
Exploring the asteroid belt with ion propulsion: Dawn mission history, status and plans
Russell, C. T., Barucci, M. A., Binzel, R. P., et al. (2007) · Advances in Space Research · doi:10.1016/j.asr.2007.05.083 · Cited by 34
“Ceres is rotationally symmetric with dimensions 487 · 487 · 455 km (Thomas et al., 2005).”
BackgroundSelf-citationPredictions for impactor contamination on Ceres based on hypervelocity impact experiments
Daly, R. T., & Schultz, P. H. (2015) · Geophysical Research Letters · doi:10.1002/2015gl065601 · Cited by 33
“However, the relatively low mean density of Ceres (~2.1 g cm 3) [Thomas et al., 2005] raises the possibility that Ceres may host significant ice [Castillo-Rogez and McCord, 2010; Castillo-Rogez, 2011] or be composed of highly porous silicates [Zolotov, 2009].”
BackgroundInfluentialGeologic mapping of the Urvara and Yalode Quadrangles of Ceres
Crown, D. A., Sizemore, H. G., Yingst, R. A., et al. (2017) · Icarus · doi:10.1016/j.icarus.2017.08.004 · Cited by 33
Self-citationHughson, K. H. G., Russell, C. T., Williams, D. A., et al. (2017) · Icarus · doi:10.1016/j.icarus.2017.09.035 · Cited by 33
Self-citationScully, J. E. C., Buczkowski, D. L., Neesemann, A., et al. (2017) · Icarus · doi:10.1016/j.icarus.2017.10.038 · Cited by 33
Self-citationPlanetesimals To Brown Dwarfs: What is a Planet?
Basri, G., & Brown, M. E. (2006) · CERN Document Server (European Organization for Nuclear Research) · Cited by 33
Drummond, J., Carry, B., Merline, W. J., et al. (2014) · Icarus · doi:10.1016/j.icarus.2014.03.038 · Cited by 32
Keihm, S. J., Kamp, L. W., Gulkis, S. L., et al. (2013) · Icarus · doi:10.1016/j.icarus.2013.07.005 · Cited by 32
Constraints on the pre-impact orbits of Solar system giant impactors
Jackson, A. P., Gabriel, T. S. J., & Asphaug, E. I. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx2901 · Cited by 29
“Ceres, the asteroid at a = 2.8 AU that contains almost half the mass of the present Main Belt, has a substantial mass fraction of water (Thomas et al. 2005; Russell et al. 2016), and more massive planetesimals, since lost from the region between Mars and Jupiter, might have had even greater water…”
BackgroundInfluentialA SEARCH FOR WATER VAPORIZATION ON CERES
Rousselot, P., Jehin, E., Manfroid, J., Mousis, O., Dumas, C., Carry, B., Marboeuf, U., & Zucconi, J. (2011) · The Astronomical Journal · doi:10.1088/0004-6256/142/4/125 · Cited by 32
“This estimate of water content is consistent with Hubble Space Telescope observations which suggest that Ceres’s shape is the result of a rocky core surrounded by an ice-rich mantle (Thomas et al. 2005).”
BackgroundResultImpactor flux and cratering on Ceres and Vesta: implications for the early solar system
de Elía, G. C., & Sisto, R. P. D. (2011) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201117543 · Cited by 31
Asteroids and the James Webb Space Telescope
Rivkin, A. S., Marchis, F., Stansberry, J., Takir, D., Thomas, C. A., & the JWST Asteroids Focus Group (2016) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/128/959/018003 · Cited by 31
“Asteroid science used the Hubble Space Telescope (HST) primarily for improved spatial resolution, as with observations of Vesta (Binzel et al. 1997; Thomas et al. 1997; Zellner et al. 1997), Ceres (Thomas et al. 2005), and Pallas (Schmidt et al. 2009).”
MethodInfluentialNeumann, W. O., Breuer, D., & Spohn, T. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201527083 · Cited by 30
“Article published by EDP Sciences A117, page 1 of 16 It should be noted that based on the shape and the moment of inertia of Ceres, no distinction between a porous and a differentiated structure is possible (Thomas et al. 2005; Carry et al. 2008).”
BackgroundEfficient early global relaxation of asteroid Vesta
Fu, R. R., Hager, B. H., Ermakov, A., et al. (2014) · Icarus · doi:10.1016/j.icarus.2014.01.023 · Cited by 29
“In contrast to Vesta, Ceres, and Pallas, the surface of Iris appears to be highly irregular at all scales >30 km with topographic relief of ∼20% of the body radius (the corresponding value for the Rheasilvia basin is ∼6%).”
BackgroundInfluentialTitus, T. N. (2015) · Geophysical Research Letters · doi:10.1002/2015gl063240 · Cited by 28
“While Ceres is no longer considered a planet by international standards, several researchers have suggested that Ceres is a differentiated body with an icy mantle and a rocky inner core [e.g., Thomas et al., 2005; McCord and Sotin, 2005; Castillo-Rogez and McCord, 2010].”
BackgroundInfluentialTechnical progress in the utilization and exploitation of small celestial body resources
Zhang, W. Y., Cheng, Q., & Li, J. (2023) · Acta Astronautica · doi:10.1016/j.actaastro.2023.03.019 · Cited by 27
Rotationally-resolved spectra of Ceres in the 3-μm region
Rivkin, A. S., & Volquardsen, E. L. (2009) · Icarus · doi:10.1016/j.icarus.2009.08.026 · Cited by 27
Rambaux, N., Chambat, F., & Castillo-Rogez, J. C. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201527005 · Cited by 26
“Finally, the analytical method of (e) Thomas et al. (2005) agrees well with the exact value of the Maclaurin equation.”
BackgroundMethodResultInfluentialCeres’s internal evolution: The view after Dawn
McCord, T. B., & Castillo-Rogez, J. C. (2018) · Meteoritics and Planetary Science · doi:10.1111/maps.13135 · Cited by 26
“H2O ice quickly sublimes at Ceres’s surface temperatures (Hayne and Aharonson 2015; Titus 2015; Formisano et al. 2016a), and thus, ice exposure must be geologically very young, perhaps 10–1000s of years, depending on amount exposed, latitude, and illumination geometry.”
BackgroundHughson, K. H. G., Russell, C. T., Schmidt, B. E., et al. (2019) · Journal of Geophysical Research Planets · doi:10.1029/2018je005666 · Cited by 26
“Ceres' low bulk density of 2162 ± 8 kg/m3 (Park et al., 2016) has long been suggestive of a composition that is rich in water ice, hydrated materials, and/or organic compounds (Castillo‐Rogez & McCord, 2010; McCord & Sotin, 2005; Russell et al., 2016; Thomas et al., 2005; Zolotov, 2009).”
BackgroundSelf-citationForced obliquities and moments of inertia of Ceres and Vesta
Bills, B. G., & Nimmo, F. (2010) · Icarus · doi:10.1016/j.icarus.2010.09.002 · Cited by 26
“If the near-surface of Ceres is ice-rich (Thomas et al., 2005), its viscoelastic relaxation (Maxwell) time will be short, perhaps even comparable to the rotation period, resulting in enhanced dissipation.”
BackgroundMethodInfluentialDyl, K. A., Cleverley, J. S., Bland, P. A., et al. (2014) · Geochimica et Cosmochimica Acta · doi:10.1016/j.gca.2014.02.020 · Cited by 25
Origin of volatiles in the main belt
Mousis, O. J., Alibert, Y., Hestroffer, D., Marboeuf, U., Dumas, C., Carry, B., Horner, J., & Selsis, F. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.12653.x · Cited by 25
“This is consistent with recent Hubble Space Telescope (HST) observations which suggest that Ceres’ shape is the result of the dwarf planet consisting of a rocky core surrounded by an ice-rich mantle (Thomas ⋆ E-mail:olivier.mousis@obs-besancon.fr et al. 2005) - an idea in agreement with several thermal evolution scena…”
BackgroundInfluentialComets, Carbonaceous Meteorites, and the Origin of the Biosphere
Hoover, R. B. (2007) · Springer eBooks · doi:10.1007/978-0-387-68656-1_4 · Cited by 25
“Thomas et al. (2005) have used the Hubble Space Telescope to investigate Ceres, the largest known asteroid.”
MethodExperimental study on compression property of regolith analogues
Omura, T., & Nakamura, A. (2017) · Planetary and Space Science · doi:10.1016/j.pss.2017.08.003 · Cited by 25
“If the same granular layer covers Ceres with its gravitational acceleration of 2.7×10-1 m/s2 based on its mass and mean radius, the thickness of the granular layer with constant porosity becomes thinner and is estimated to 1.50±0.2 m (Thomas et al., 2005).”
BackgroundInfluentialMao, X., & McKinnon, W. B. (2017) · Icarus · doi:10.1016/j.icarus.2017.08.033 · Cited by 24
Ceres, Vesta, and Pallas: Protoplanets, not asteroids
McCord, T. B., McFadden, L. A., Russell, C. T., et al. (2006) · Eos · doi:10.1029/2006eo100002 · Cited by 24
Self-citationThe nucleus of main-belt Comet P/2010 R2 (La Sagra)
Hsieh, H. (2014) · Icarus · doi:10.1016/j.icarus.2014.08.033 · Cited by 23
“…recent discoveries of corroborating evidence of water ice in the asteroid belt, however, it is important to note that Ceres (952 km in diameter Thomas et al., 2005), Themis (202 km in diameter; Wright et al., 2010; Mainzer et al., 2011; Masiero et al., 2011) and Cybele (273 km in diameter;…”
BackgroundLandslides on Ceres: Inferences Into Ice Content and Layering in the Upper Crust
Chilton, H., Schmidt, B. E., Duarte, K. D., et al. (2019) · Journal of Geophysical Research Planets · doi:10.1029/2018je005634 · Cited by 23
“…agree well with other observations by the Dawn spacecraft that suggest the presence of significant ice. Ceres' outer 190‐km shell has a density of 1,680–1,950 kg/m3 (Park et al., 2016), consistent with pre‐Dawn estimates of 16–27% ice by mass (McCord & Sotin, 2005; Thomas et al., 2005).”
BackgroundSelf-citationThe Size and Shape of the Oblong Dwarf Planet Haumea
Lockwood, A. C., Brown, M. E., Brown, M. E., et al. (2015) · Cited by 23
Photometric properties of Ceres from telescopic observations using Dawn Framing Camera color filters
Reddy, V., Li, J., Gary, B. L., et al. (2015) · Icarus · doi:10.1016/j.icarus.2015.06.039 · Cited by 23
The Effect of Semicollisional Accretion on Planetary Spins
Schlichting, H. E., & Sari, R. (2007) · The Astrophysical Journal · doi:10.1086/511129 · Cited by 23
“Ceres’s spin axis has a 12 inclination with respect to the normal of the ecliptic (Thomas et al. 2005), and Vesta’s spin axis inclination to the normal of the ecliptic is 40 (Drummond et al. 1998).”
BackgroundThe effect of Semi-Collisional Accretion on Planetary Spins
Schlichting, H. E., & Sari, R. (2006) · CERN Document Server (European Organization for Nuclear Research) · Cited by 23
Constraints on an exosphere at Ceres from Hubble Space Telescope observations
Roth, L., Ivchenko, N., Retherford, K. D., et al. (2016) · Geophysical Research Letters · doi:10.1002/2015gl067451 · Cited by 22
“…sublimation derived, the source rate for sublimation of H2O and hence the exospheric density ultimately depend on the amount of ice that is either actually exposed at the surface or only covered by a very thin layer of nonice material [Fanale and Salvail, 1989; Titus, 2015; Formisano et al., 2015].”
BackgroundLandslide Morphology and Mobility on Ceres Controlled by Topography
Johnson, B. C., & Sori, M. M. (2020) · Journal of Geophysical Research Planets · doi:10.1029/2020je006640 · Cited by 22
Submillimeter photometry and lightcurves of Ceres and other large asteroids
Chamberlain, M. A., Lovell, A. J., & Sykes, M. V. (2009) · Icarus · doi:10.1016/j.icarus.2009.03.002 · Cited by 21
Self-citationHessel, V., Tran, N. N., Orandi, S., Asrami, M. R., Goodsite, M. E., & Nguyen, H. (2020) · Angewandte Chemie International Edition · doi:10.1002/anie.201912205 · Cited by 23
The morphologic and morphometric characteristics of craters on Ceres and implications for the crust
Zeilnhofer, M. F., & Barlow, N. G. (2021) · Icarus · doi:10.1016/j.icarus.2021.114428 · Cited by 22
Dynamical origin of the Dwarf Planet Ceres
de Sousa, R. R., Morbidelli, A., Gomes, R. S., Neto, E. V., Izidoro, A., & Alves, A. A. (2022) · Icarus · doi:10.1016/j.icarus.2022.114933 · Cited by 22
“The interior structure of Ceres comprises a water-ice-rich mantle over a rock core, with a bulk rock-ice fraction of 75%-25% respectively (Thomas et al. 2005).”
BackgroundDynamical delivery of volatiles to the outer main belt
Grazier, K. R., Castillo-Rogez, J. C., & Sharp, P. W. (2013) · Icarus · doi:10.1016/j.icarus.2013.12.011 · Cited by 19
True polar wander of Ceres due to heterogeneous crustal density
Tricarico, P. (2018) · Nature Geoscience · doi:10.1038/s41561-018-0232-3 · Cited by 19
Molaro, P. P., & Centurión, M. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201015179 · Cited by 18
“Ceres is rotationally symmetric to the limit of measurement accuracy and can be described by an oblate spheroid of axes a = 487.3 ± 1.6 and b = 454.7 ± 1.6 km (Thomas et al. 2005).”
BackgroundInfluentialA Sublimation-driven Exospheric Model of Ceres
Tu, L., Ip, W., & Wang, Y.-C. (2014) · Planetary and Space Science · doi:10.1016/j.pss.2014.09.002 · Cited by 18
Constraining Ceres ’ interior from its Rotational Motion
Rambaux, N., Castillo-Rogez, J. C., Dehant, V., et al. (2011) · Cited by 18
Origin and Evolution of Volatile-rich Asteroids
Castillo-Rogez, J. C., & Young, E. (2017) · Cambridge University Press eBooks · doi:10.1017/9781316339794.005 · Cited by 18
“the observation of its global shape obtained with the Hubble Space Telescope (Thomas et al., 2005) and adaptive optics (e.”
MethodSelf-citationRadius and limb topography of Mercury obtained from images acquired during the MESSENGER flybys
Oberst, J., Elgner, S., Turner, F. S., et al. (2011) · Planetary and Space Science · doi:10.1016/j.pss.2011.07.003 · Cited by 17
Shepard, M. K. (2015) · Cambridge University Press eBooks · doi:10.1017/cbo9781107447899 · Cited by 18
Origin of volatiles in the main belt
Mousis, O. J., Alibert, Y., Hestroffer, D., Marboeuf, U., Dumas, C., Carry, B., Horner, J., & Selsis, F. (2008) · University of Southern Queensland ePrints (University of Southern Queensland) · doi:10.7892/boris.36909 · Cited by 17
Burbine, T. H., Rivkin, A. S., NOBLE, S. K., Mothé-Diniz, T., Bottke, W. F., McCoy, T. J., Dyar, M. D., & Thomas, C. A. (2008) · Reviews in Mineralogy and Geochemistry · doi:10.2138/rmg.2008.68.12 · Cited by 17
“Asteroid 1 Ceres, a member of the C-complex, is the largest object in the main belt (975 by 909 km) (Thomas et al. 2005).”
BackgroundCastro-Chávez, F. (2011) · NeuroQuantology · doi:10.14704/nq.2011.9.4.500 · Cited by 17
“Evidence of both glacial ages and of waters arriving from outside the Earth to drawn it, remaining on it most specially the ones from the second flooding, I think, are the waters found in the dark side of the moon (Colaprete et al., 2010), where its dark pole is located (Duke, 2002), and in the south pole of mars (Mac…”
BackgroundInfluentialDawn at Ceres: The first exploration of the first dwarf planet discovered
Rayman, M. D. (2019) · Acta Astronautica · doi:10.1016/j.actaastro.2019.12.017 · Cited by 16
Short-term variability on the surface of (1) Ceres
Perna, D., Kaňuchová, Z., Ieva, S., et al. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201425304 · Cited by 16
“Themodeling of the thermo-physico-chemical evolution of Ceres, which is constrained by the available shape and density measurements (2077±36 kg m−3, Thomas et al. 2005; 2206±43 kg m−3, Carry et al. 2008), points to a differentiated interior.”
BackgroundWater, heat, bombardment: The evolution and current state of (2) Pallas
Schmidt, B. E., & Castillo-Rogez, J. C. (2011) · Icarus · doi:10.1016/j.icarus.2011.11.019 · Cited by 17
Bhatia, G. K., & Sahijpal, S. (2017) · Meteoritics and Planetary Science · doi:10.1111/maps.12952 · Cited by 15
“Aside from the icy satellites and the icyrocky cores of the giant planets, trans-Neptunian objects (TNOs) and icy minor planets, e.g., Ceres, Pluto, etc. (Thomas et al. 2005), are also considered to have formed and evolved in the early solar system.”
BackgroundFormation of Vitreous Salt Hydrates Under Conditions Relevant to Europa
Johnson, P. V., & Vu, T. H. (2022) · The Planetary Science Journal · doi:10.3847/psj/ac6bfb · Cited by 14
Calathus: A sample-return mission to Ceres
Gassot, O., Panicucci, P., Acciarini, G., et al. (2021) · Acta Astronautica · doi:10.1016/j.actaastro.2020.12.050 · Cited by 14
The Explored Asteroids: Science and Exploration in the Space Age
Sears, D. W. G. (2015) · Space Science Reviews · doi:10.1007/s11214-015-0202-7 · Cited by 13
Onset of oligarchic growth and implication for accretion histories of dwarf planets
Morishima, R. (2016) · Icarus · doi:10.1016/j.icarus.2016.07.019 · Cited by 13
“7, we overplot the masses of Vesta (Russell et al., 2012) and the five dwarf planets recognized by the IAU as of January 2016: Ceres (Thomas et al., 2005, and references therein), Pluto (Stern et al., 2015), Haumea (Ragozzine and Brown, 2009), Makemake (Brown, 2013, we assumed ρ = 2.3 g cm−3), and…”
MethodInfluentialThe stability of the crust of the dwarf planet Ceres
Formisano, V., Federico, C., Angelis, S. D., Sanctis, M. C. D., & Magni, G. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1910 · Cited by 13
Shoji, D., & Kurita, K. (2014) · Journal of Geophysical Research Planets · doi:10.1002/2014je004695 · Cited by 13
An, M., Wang, Z., & Zhang, Y. (2016) · Acta Astronautica · doi:10.1016/j.actaastro.2016.10.038 · Cited by 13
Gas–solid carbonation as a possible source of carbonates in cold planetary environments
Garenne, A., Montes-Hernandez, G., Beck, P., Schmitt, B., Brissaud, O., & Pommerol, A. (2012) · Planetary and Space Science · doi:10.1016/j.pss.2012.11.005 · Cited by 14
“equilibrium and its bulk density suggests the presence of ice in its interior (Thomas et al., 2005).”
BackgroundCeres: High-resolution imaging with HST and the determination of physical properties
Parker, J. W., McFadden, L. A., Russell, C. T., et al. (2005) · Advances in Space Research · doi:10.1016/j.asr.2004.12.040 · Cited by 13
Self-citationThe remarkable surface homogeneity of the Dawn mission target (1) Ceres
Carry, B., Vernazza, P., Dumas, C., et al. (2011) · Icarus · doi:10.1016/j.icarus.2011.10.015 · Cited by 12
“…for instance), Ceres recently has been the sub-17 ject of increased attention from the community (e.g., Parker 18 et al. 2002, Nazzario et al. 2003, Thomas et al. 2005, Vernazza 19 et al. 2005, McCord and Sotin 2005, Li et al. 2006, Rivkin et al. 20 2006, Chamberlain et al. 2007, Kovačević and…”
BackgroundInfluentialAsteroids: New Challenges, New Targets
Libourel, G., & Corrigan, C. M. (2014) · Elements · doi:10.2113/gselements.10.1.11 · Cited by 11
Short-term variability on the surface of (1) Ceres. A changing amount of water ice?Preprint
Perna, D., Kaňuchová, Z., Ieva, S., et al. (2014) · arXiv (Cornell University) · doi:10.48550/arxiv.1412.5318 · Cited by 12
“Themodeling of the thermo-physico-chemical evolution of Ceres, which is constrained by the available shape and density measurements (2077±36 kg m−3, Thomas et al. 2005; 2206±43 kg m−3, Carry et al. 2008), points to a differentiated interior.”
BackgroundIntroduction to the special issue: The formation and evolution of Ceres’ Occator crater
Scully, J. E. C., Russell, C. T., Castillo-Rogez, J. C., et al. (2018) · Icarus · doi:10.1016/j.icarus.2018.02.029 · Cited by 12
Self-citationCeres’ rotation solution under the gravitational torque of the Sun
Lara, M., Fukushima, T., & Ferrer, S. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.18717.x · Cited by 11
“However, as highlighted by Castillo-Rogez & McCord (2010), non-negligible differences of several km in its mean radius are found in the works of Carry et al. (2008) and Thomas et al. (2005), despite both works claiming a similar measurement uncertainty of about 2 km.”
BackgroundMethodResultInfluentialVesta and Ceres: Crossing the History of the Solar System
Coradini, A., Turrini, D., Federico, C., & Magni, G. (2011) · Springer eBooks · doi:10.1007/978-1-4614-4903-4_3 · Cited by 11
The Dawn Topography Investigation
Raymond, C. A., Jaumann, R., Nathues, A., et al. (2011) · Springer eBooks · doi:10.1007/978-1-4614-4903-4_16 · Cited by 11
Results of two multichord stellar occultations by dwarf planet (1) Ceres
Gomes-Júnior, A. R., Giacchini, B. L., Braga-Ribas, F., et al. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1081 · Cited by 11
“We note an overall agreement between our result to those obtained via direct imaging by the Hubble Space Telescope (HST) (Thomas et al. 2005), the Keck Observatory and the ESO VLT (Drummond et al. 2014).”
ResultA new equation of state applied to planetary impacts
Wissing, R., & Hobbs, D. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201936227 · Cited by 11
Sierks, H., Keller, H. U., Jaumann, R., et al. (2011) · Springer eBooks · doi:10.1007/978-1-4614-4903-4_12 · Cited by 11
Ptolemy operations and results during the Lutetia flyby
Andrews, D. J., Morse, A. D., Barber, S. J., et al. (2011) · Planetary and Space Science · doi:10.1016/j.pss.2011.09.005 · Cited by 11
The proposed Caroline ESA M3 mission to a Main Belt Comet
Jones, G. H., Agarwal, J., Bowles, N. E., Burchell, M. J., Coates, A. J., Fitzsimmons, A., Graps, A. L., Hsieh, H. H., Lisse, C. M., Lowry, S. C., et al. (2018) · Advances in Space Research · doi:10.1016/j.asr.2018.02.032 · Cited by 12
Ceres, a wet planet: The view after Dawn
McCord, T. B., Combe, J., Castillo-Rogez, J. C., McSWEEN, H. Y., Jr., & Prettyman, T. H. (2021) · Geochemistry · doi:10.1016/j.chemer.2021.125745 · Cited by 10
Ceres interaction with the solar wind
Lindkvist, J., Holmström, M., Fatemi, S., et al. (2017) · Geophysical Research Letters · doi:10.1002/2016gl072375 · Cited by 10
“Ceres has a mean radius of R=476.2 km [Thomas et al., 2005], and mass M=9.324 ⋅ 1020 kg [Küppers et al., 2014].”
Influential
Metadata
- 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 › Earth and Planetary Sciences › Space and Planetary Science › Astro and Planetary Science
- Physical Sciences › Earth and Planetary Sciences › Space and Planetary Science › 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
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
What counts as a claim ›How we measure confidence ›How we check this ›
Are you an author, or do you see a problem with this page? Request a review
