Ceres (dwarf planet)
|Discovered by||Giuseppe Piazzi|
|Discovery date||1 January 1801|
|MPC designation||(1) Ceres|
|A899 OF; 1943 XB|
rarely Cererean //
|Aphelion||2.9773 AU |
|Perihelion||2.5577 AU |
|2.7675 AU |
Average orbital speed
|Inclination||10.593° to ecliptic|
9.20° to invariable plane
|Proper orbital elements|
Proper semi-major axis
Proper mean motion
|78.193318 deg / yr|
Proper orbital period
Precession of perihelion
|54.070272 arcsec / yr|
Precession of the ascending node
|−59.170034 arcsec / yr|
|Dimensions||(965.2 × 961.2|
× 891.2) ± 2.0 km
Equatorial surface gravity
Equatorial escape velocity
Sidereal rotation period
Equatorial rotation velocity
North pole right ascension
North pole declination
|6.64 to 9.34|
|0.854″ to 0.339″|
Ceres (//; minor-planet designation: 1 Ceres) is the largest object in the asteroid belt that lies between the orbits of Mars and Jupiter, slightly closer to Mars's orbit. With a diameter of 945 km (587 mi), Ceres is both the largest of the asteroids and the only unambiguous dwarf planet inside Neptune's orbit. It is the 33rd-largest known body in the Solar System.[c]
Ceres is composed of rock and ice, and contains approximately one-third of the mass of the entire asteroid belt. Ceres is the only object in the asteroid belt known to be rounded by its own gravity, although detailed analysis was required to exclude Vesta. From Earth, the apparent magnitude of Ceres ranges from 6.7 to 9.3, peaking once at opposition every 15 to 16 months, which is its synodic period. Thus even at its brightest, it is too dim to be seen by the naked eye, except under extremely dark skies.
Ceres was the first asteroid to be discovered (by Giuseppe Piazzi at Palermo Astronomical Observatory on 1 January 1801). It was originally considered a planet, but was reclassified as an asteroid in the 1850s after many other objects in similar orbits were discovered.
Ceres appears to be differentiated into a rocky core and an icy mantle, and may have a remnant internal ocean of liquid water under the layer of ice. The surface is a mixture of water ice and various hydrated minerals such as carbonates and clay. In January 2014, emissions of water vapor were detected from several regions of Ceres. This was unexpected because large bodies in the asteroid belt typically do not emit vapor, a hallmark of comets.
The robotic NASA spacecraft Dawn entered orbit around Ceres on 6 March 2015. Pictures with a resolution previously unattained were taken during imaging sessions starting in January 2015 as Dawn approached Ceres, showing a cratered surface. Two distinct bright spots (or high-albedo features) inside a crater (different from the bright spots observed in earlier Hubble images) were seen in a 19 February 2015 image, leading to speculation about a possible cryovolcanic origin or outgassing. On 3 March 2015, a NASA spokesperson said the spots are consistent with highly reflective materials containing ice or salts, but that cryovolcanism is unlikely. However, on 2 September 2016, scientists from the Dawn team claimed in a Science paper that a massive cryovolcano called Ahuna Mons is the strongest evidence yet for the existence of these mysterious formations. On 11 May 2015, NASA released a higher-resolution image showing that, instead of one or two spots, there are actually several. On 9 December 2015, NASA scientists reported that the bright spots on Ceres may be related to a type of salt, particularly a form of brine containing magnesium sulfate hexahydrite (MgSO4·6H2O); the spots were also found to be associated with ammonia-rich clays. In June 2016, near-infrared spectra of these bright areas were found to be consistent with a large amount of sodium carbonate (Na
3), implying that recent geologic activity was probably involved in the creation of the bright spots. In July 2018, NASA released a comparison of physical features found on Ceres with similar ones present on Earth. From June to October 2018, Dawn orbited Ceres from as close as 35 km (22 mi) and as far away as 4,000 km (2,500 mi). The Dawn mission ended on 1 November 2018 after the spacecraft ran out of fuel.
- 1 History
- 2 Orbit
- 3 Rotation and axial tilt
- 4 Geology
- 5 Atmosphere
- 6 Origin and evolution
- 7 Potential habitability
- 8 Observation and exploration
- 9 Maps
- 10 Gallery
- 11 See also
- 12 Notes
- 13 References
- 14 External links
Johann Elert Bode, in 1772, first suggested that an undiscovered planet could exist between the orbits of Mars and Jupiter. Kepler had already noticed the gap between Mars and Jupiter in 1596. Bode based his idea on the Titius–Bode law which is a now-discredited hypothesis that was first proposed in 1766. Bode observed that there was a regular pattern in the size of the orbits of known planets, and that the pattern was marred only by the large gap between Mars and Jupiter. The pattern predicted that the missing planet ought to have an orbit with a radius near 2.8 astronomical units (AU). William Herschel's discovery of Uranus in 1781 near the predicted distance for the next body beyond Saturn increased faith in the law of Titius and Bode, and in 1800, a group headed by Franz Xaver von Zach, editor of the Monatliche Correspondenz, sent requests to twenty-four experienced astronomers (whom he dubbed the "celestial police"), asking that they combine their efforts and begin a methodical search for the expected planet. Although they did not discover Ceres, they later found several large asteroids.
One of the astronomers selected for the search was Giuseppe Piazzi, a Catholic priest at the Academy of Palermo, Sicily. Before receiving his invitation to join the group, Piazzi discovered Ceres on 1 January 1801. He was searching for "the 87th [star] of the Catalogue of the Zodiacal stars of Mr la Caille", but found that "it was preceded by another". Instead of a star, Piazzi had found a moving star-like object, which he first thought was a comet. Piazzi observed Ceres a total of 24 times, the final time on 11 February 1801, when illness interrupted his observations. He announced his discovery on 24 January 1801 in letters to only two fellow astronomers, his compatriot Barnaba Oriani of Milan and Johann Elert Bode of Berlin. He reported it as a comet but "since its movement is so slow and rather uniform, it has occurred to me several times that it might be something better than a comet". In April, Piazzi sent his complete observations to Oriani, Bode, and Jérôme Lalande in Paris. The information was published in the September 1801 issue of the Monatliche Correspondenz.
By this time, the apparent position of Ceres had changed (mostly due to Earth's orbital motion), and was too close to the Sun's glare for other astronomers to confirm Piazzi's observations. Toward the end of the year, Ceres should have been visible again, but after such a long time it was difficult to predict its exact position. To recover Ceres, Carl Friedrich Gauss, then 24 years old, developed an efficient method of orbit determination. In only a few weeks, he predicted the path of Ceres and sent his results to von Zach. On 31 December 1801, von Zach and Heinrich W. M. Olbers found Ceres near the predicted position and thus recovered it.
The early observers were only able to calculate the size of Ceres to within an order of magnitude. Herschel underestimated its diameter as 260 km in 1802, whereas in 1811 Johann Hieronymus Schröter overestimated it as 2,613 km.
Piazzi originally suggested the name Cerere Ferdinandea for his discovery, after the goddess Ceres (Roman goddess of agriculture, Cerere in Italian, who was believed to have originated in Sicily and whose oldest temple was there) and King Ferdinand of Sicily. "Ferdinandea", however, was not acceptable to other nations and was dropped. Ceres was called Hera for a short time in Germany. In Greece, it is called Demeter (Δήμητρα), after the Greek equivalent of the Roman Cerēs;[d] in English, that name is used for the asteroid 1108 Demeter.
The regular adjectival forms of the name are Cererian and Cererean, derived from the Latin genitive Cereris, but Ceresian is occasionally seen for the goddess (as in the sickle-shaped Ceresian Lake), as is the shorter form Cerean.
The old astronomical symbol of Ceres is a sickle, ⟨⚳⟩ (), similar to Venus' symbol ⟨♀⟩ but with a break in the circle. It has a variant ⟨ ⟩, reversed under the influence of the initial letter 'C' of 'Ceres'. These were later replaced with the generic asteroid symbol of a numbered disk, ⟨①⟩.
Cerium, a rare-earth element discovered in 1803, was named after Ceres.[e] In the same year another element was also initially named after Ceres, but when cerium was named, its discoverer changed the name to palladium, after the second asteroid, 2 Pallas.
The categorization of Ceres has changed more than once and has been the subject of some disagreement. Johann Elert Bode believed Ceres to be the "missing planet" he had proposed to exist between Mars and Jupiter, at a distance of 419 million km (2.8 AU) from the Sun. Ceres was assigned a planetary symbol, and remained listed as a planet in astronomy books and tables (along with 2 Pallas, 3 Juno, and 4 Vesta) for half a century.
As other objects were discovered in the neighborhood of Ceres, it was realized that Ceres represented the first of a new class of objects. In 1802, with the discovery of 2 Pallas, William Herschel coined the term asteroid ("star-like") for these bodies, writing that "they resemble small stars so much as hardly to be distinguished from them, even by very good telescopes". As the first such body to be discovered, Ceres was given the designation 1 Ceres under the modern system of minor-planet designations. By the 1860s, the existence of a fundamental difference between asteroids such as Ceres and the major planets was widely accepted, though a precise definition of "planet" was never formulated.
The 2006 debate surrounding Pluto and what constitutes a planet led to Ceres being considered for reclassification as a planet. A proposal before the International Astronomical Union for the definition of a planet would have defined a planet as "a celestial body that (a) has sufficient mass for its self-gravity to overcome rigid-body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and (b) is in orbit around a star, and is neither a star nor a satellite of a planet". Had this resolution been adopted, it would have made Ceres the fifth planet in order from the Sun. This never happened, however, and on 24 August 2006 a modified definition was adopted, carrying the additional requirement that a planet must have "cleared the neighborhood around its orbit". By this definition, Ceres is not a planet because it does not dominate its orbit, sharing it as it does with the thousands of other asteroids in the asteroid belt and constituting only about a third of the mass of the belt. Bodies that met the first proposed definition but not the second, such as Ceres, were instead classified as dwarf planets.
Ceres is the largest object in the asteroid belt. It is sometimes assumed that Ceres has been reclassified as a dwarf planet, and that it is therefore no longer considered an asteroid. For example, a news update at Space.com spoke of "Pallas, the largest asteroid, and Ceres, the dwarf planet formerly classified as an asteroid", whereas an IAU question-and-answer posting states, "Ceres is (or now we can say it was) the largest asteroid", though it then speaks of "other asteroids" crossing Ceres' path and otherwise implies that Ceres is still considered an asteroid. The Minor Planet Center notes that such bodies may have dual designations. The 2006 IAU decision that classified Ceres as a dwarf planet never addressed whether it is or is not an asteroid. Indeed, the IAU has never defined the word 'asteroid' at all, having preferred the term 'minor planet' until 2006, and preferring the terms 'small Solar System body' and 'dwarf planet' after 2006. Lang (2011) comments "the [IAU has] added a new designation to Ceres, classifying it as a dwarf planet. ... By [its] definition, Eris, Haumea, Makemake and Pluto, as well as the largest asteroid, 1 Ceres, are all dwarf planets", and describes it elsewhere as "the dwarf planet–asteroid 1 Ceres". NASA continues to refer to Ceres as an asteroid, as do various academic textbooks.
(Epoch 23 July 2010 )
Ceres follows an orbit between Mars and Jupiter, within the asteroid belt, with a period of 4.6 Earth years. The orbit is moderately inclined (i = 10.6° compared to 7° for Mercury and 17° for Pluto) and moderately eccentric (e = 0.08 compared to 0.09 for Mars).
The diagram illustrates the orbits of Ceres (blue) and several planets (white and gray). The segments of orbits below the ecliptic are plotted in darker colors, and the orange plus sign is the Sun's location. The top left diagram is a polar view that shows the location of Ceres in the gap between Mars and Jupiter. The top right is a close-up demonstrating the locations of the perihelia (q) and aphelia (Q) of Ceres and Mars. In this diagram (but not in general), the perihelion of Mars is on the opposite side of the Sun from those of Ceres and several of the large main-belt asteroids, including 2 Pallas and 10 Hygiea. The bottom diagram is a side view showing the inclination of the orbit of Ceres compared to the orbits of Mars and Jupiter.
Ceres was once thought to be a member of an asteroid family. The asteroids of this family share similar proper orbital elements, which may indicate a common origin through an asteroid collision some time in the past. Ceres was later found to have spectral properties different from other members of the family, which is now called the Gefion family after the next-lowest-numbered family member, 1272 Gefion. Ceres appears to be merely an interloper in the Gefion family, coincidentally having similar orbital elements but not a common origin.
Ceres is in a near-1:1 mean-motion orbital resonance with Pallas (their proper orbital periods differ by 0.2%). However, a true resonance between the two would be unlikely; due to their small masses relative to their large separations, such relationships among asteroids are very rare. Nevertheless, Ceres is able to capture other asteroids into temporary 1:1 resonant orbital relationships (making them temporary trojans) for periods up to 2 million years or more; fifty such objects have been identified.
Transits of planets from Ceres
Mercury, Venus, Earth, and Mars can all appear to cross the Sun, or transit it, from a vantage point on Ceres. The most common transits are those of Mercury, which usually happen every few years, most recently in 2006 and 2010. The most recent transit of Venus was in 1953, and the next will be in 2051; the corresponding dates are 1814 and 2081 for transits of Earth, and 767 and 2684 for transits of Mars.
Rotation and axial tilt
The rotation period of Ceres (the Cererian day) is 9 hours and 4 minutes. It has an axial tilt of 4°. This is small enough for Ceres's polar regions to contain permanently shadowed craters that are expected to act as cold traps and accumulate water ice over time, similar to the situation on the Moon and Mercury. About 0.14% of water molecules released from the surface are expected to end up in the traps, hopping an average of 3 times before escaping or being trapped.
Ceres has a mass of 9.39×1020 kg as determined from the Dawn spacecraft. With this mass Ceres composes approximately a third of the estimated total 3.0 ± 0.2×1021 kg mass of the asteroid belt, which is in turn approximately 4% of the mass of the Moon. Ceres is massive enough to give it a nearly spherical, equilibrium shape. Among Solar System bodies, Ceres is intermediate in size between the smaller Vesta and the larger Tethys. Its surface area is approximately the same as the land area of India or Argentina. In July 2018, NASA released a comparison of physical features found on Ceres with similar ones present on Earth.
Ceres is the smallest object confirmed to be in hydrostatic equilibrium, being 600 km smaller and less than half the mass of Saturn's moon Rhea, the next smallest such object. Modeling has suggested Ceres could have a small metallic core from partial differentiation of its rocky fraction.
The surface composition of Ceres is broadly similar to that of C-type asteroids. Some differences do exist. The ubiquitous features in Ceres' IR spectrum are those of hydrated materials, which indicate the presence of significant amounts of water in its interior. Other possible surface constituents include iron-rich clay minerals (cronstedtite) and carbonate minerals (dolomite and siderite), which are common minerals in carbonaceous chondrite meteorites. The surface rock appears to have many pores filled with water ice, ∼ 10% by weight. The spectral features of carbonates and clay minerals are usually absent in the spectra of other C-type asteroids. Sometimes Ceres is classified as a G-type asteroid.
Ceres' surface is relatively warm. The maximum temperature with the Sun overhead was estimated from measurements to be 235 K (approximately −38 °C, −36 °F) on 5 May 1991. Ice sublimates at this temperature in the near vacuum. Material left behind by the sublimation of surface ice could explain the dark surface of Ceres compared to the icy moons of the outer Solar System.
Studies by the Hubble Space Telescope reveal that graphite, sulfur, and sulfur dioxide are present on Ceres's surface. The former is evidently the result of space weathering on Ceres's older surfaces; the latter two are volatile under Cererian conditions and would be expected to either escape quickly or settle in cold traps, and are evidently associated with areas with recent geological activity.
Observations prior to Dawn
Prior to the Dawn mission, only a few surface features had been unambiguously detected on Ceres. High-resolution ultraviolet Hubble Space Telescope images taken in 1995 showed a dark spot on its surface, which was nicknamed "Piazzi" in honor of the discoverer of Ceres. This was thought to be a crater. Later near-infrared images with a higher resolution taken over a whole rotation with the Keck telescope using adaptive optics showed several bright and dark features moving with Ceres' rotation. Two dark features had circular shapes and were presumed to be craters; one of them was observed to have a bright central region, whereas another was identified as the "Piazzi" feature. Visible-light Hubble Space Telescope images of a full rotation taken in 2003 and 2004 showed eleven recognizable surface features, the natures of which were then undetermined. One of these features corresponds to the "Piazzi" feature observed earlier.
These last observations indicated that the north pole of Ceres pointed in the direction of right ascension 19 h 24 min (291°), declination +59°, in the constellation Draco, resulting in an axial tilt of approximately 3°. Dawn later determined that the north polar axis actually points at right ascension 19 h 25 m 40.3 s (291.418°), declination +66° 45' 50" (about 1.5 degrees from Delta Draconis), which means an axial tilt of 4°.
Observations by Dawn
Dawn revealed that Ceres has a heavily cratered surface; nevertheless, Ceres does not have as many large craters as expected, likely due to past geological processes. An unexpectedly large number of Cererian craters have central pits, perhaps due to cryovolcanic processes, and many have central peaks. Ceres has one prominent mountain, Ahuna Mons; this peak appears to be a cryovolcano and has few craters, suggesting a maximum age of no more than a few hundred million years. A later computer simulation has suggested that there were originally other cryovolcanoes on Ceres that are now unrecognisable due to viscous relaxation. Several bright spots have been observed by Dawn, the brightest spot ("Spot 5") located in the middle of an 80-kilometer (50 mi) crater called Occator. From images taken of Ceres on 4 May 2015, the secondary bright spot was revealed to actually be a group of scattered bright areas, possibly as many as ten. These bright features have an albedo of approximately 40% that are caused by a substance on the surface, possibly ice or salts, reflecting sunlight. A haze periodically appears above Spot 5, the best known bright spot, supporting the hypothesis that some sort of outgassing or sublimating ice formed the bright spots. In March 2016, Dawn found definitive evidence of water molecules on the surface of Ceres at Oxo crater.
On 9 December 2015, NASA scientists reported that the bright spots on Ceres may be related to a type of salt, particularly a form of brine containing magnesium sulfate hexahydrite (MgSO4·6H2O); the spots were also found to be associated with ammonia-rich clays. Near-infrared spectra of these bright areas were reported in 2017 to be consistent with a large amount of sodium carbonate (Na
3) and smaller amounts of ammonium chloride (NH
4Cl) or ammonium bicarbonate (NH
3). These materials have been suggested to originate from the recent crystallization of brines that reached the surface from below.
Organic compounds (tholins) were detected on Ceres in Ernutet crater, and most of the planet's surface is extremely rich in carbon, with approximately 20% carbon by mass in its near surface. The carbon content is more than five times higher than in carbonaceous chondrite meteorites analyzed on Earth. The surface carbon shows evidence of being mixed with products of rock-water interactions, such as clays. This chemistry suggests Ceres formed in a cold environment, perhaps outside the orbit of Jupiter, and that it accreted from ultra-carbon-rich materials in the presence of water, which could provide conditions favorable to organic chemistry. Its presence on Ceres is evidence that the basic ingredients for life can be found throughout the universe.
"Spot 1" (top row) ("cooler" than surroundings);
"Spot 5" (bottom) ("similar in temperature" as surroundings) (April 2015)
This article needs to be updated.April 2019)(
Ceres is thought to consist of a rocky core overlain with an icy mantle and crust. Shape (oblateness) and gravity-field measurements by Dawn confirm that Ceres is in hydrostatic equilibrium and is partially differentiated, with isostatic compensation and a mean moment of inertia of 0.37 (which is similar to that of Callisto at ~0.36). Ceres may be up to 25% water by mass, which is more water than there is on Earth.[better ref needed]
One study estimated the densities of the core and mantle/crust to be 2.46–2.90 and 1.68–1.95 g/cm3, with the mantle and crust being 70–190 km thick. Only partial dehydration (expulsion of ice) from the core is expected, while the high density of the mantle relative to water ice reflects its enrichment in silicates and salts. That is, the core, mantle and crust all consist of rock and ice, though in different ratios.
A second study modeled Ceres as having two layers, a core of chondrules and a mantle of mixed ice and micron-sized solid particulates ("mud"). Sublimation of ice at the surface would leave a deposit of hydrated particulates perhaps 20 meters thick. There are range to the extent of differentiation that is consistent with the data, from a large, 360-km core of 75% chondrules and 25% particulates and a mantle of 75% ice and 25% particulates, to a small, 85-km core consisting nearly entirely of particulates and a mantle of 30% ice and 70% particulates. With a large core, the core–mantle boundary should be warm enough for pockets of brine. With a small core, the mantle should remain liquid below 110 km. In the latter case, a 2% freezing of the liquid reservoir would compress the liquid enough to force some to the surface, producing cryovolcanism. This may be compared to estimates that Ceres has averaged one cryovolcano every 50 million years.
The mineral composition can only be determined indirectly for the outer 100 km. The 40-km thick solid outer crust is a mixture of ice, salts, and hydrated minerals. Under that is a layer that may contain a small amount of brine. This extends to a depth of at least the 100-km limit of detection. Under that is thought to be a mantle dominated by hydrated rocks such as clays. It is not possible to tell if Ceres' deep interior contains liquid or a core of dense material rich in metal.
Surface water ice is unstable at distances less than 5 AU from the Sun, so it is expected to sublime if it is exposed directly to solar radiation. Water ice can migrate from the deep layers of Ceres to the surface, but escapes in a very short time. As a result, it is difficult to detect water vaporization. Water escaping from polar regions of Ceres was possibly observed in the early 1990s but this has not been unambiguously demonstrated. It may be possible to detect escaping water from the surroundings of a fresh impact crater or from cracks in the subsurface layers of Ceres. Ultraviolet observations by the IUE spacecraft detected statistically significant amounts of hydroxide ions near Ceres' north pole, which is a product of water vapor dissociation by ultraviolet solar radiation.
In early 2014, using data from the Herschel Space Observatory, it was discovered that there are several localized (not more than 60 km in diameter) mid-latitude sources of water vapor on Ceres, which each give off approximately 1026 molecules (or 3 kg) of water per second.[f] Two potential source regions, designated Piazzi (123°E, 21°N) and Region A (231°E, 23°N), have been visualized in the near infrared as dark areas (Region A also has a bright center) by the W. M. Keck Observatory. Possible mechanisms for the vapor release are sublimation from approximately 0.6 km2 of exposed surface ice, or cryovolcanic eruptions resulting from radiogenic internal heat or from pressurization of a subsurface ocean due to growth of an overlying layer of ice. Surface sublimation would be expected to be lower when Ceres is farther from the Sun in its orbit, whereas internally powered emissions should not be affected by its orbital position. The limited data available was more consistent with cometary-style sublimation; however, subsequent evidence from Dawn strongly suggests ongoing geologic activity could be at least partially responsible.
Studies using Dawn's gamma ray and neutron detector (GRaND) reveal that Ceres is accelerating electrons from the solar wind regularly; although there are several possibilities as to what is causing this, the most accepted is that these electrons are being accelerated by collisions between the solar wind and a tenuous water vapor exosphere.
In 2017, Dawn confirmed that Ceres has a transient atmosphere that appears to be linked to solar activity. Ice on Ceres can sublimate when energetic particles from the Sun hit exposed ice within craters.
Origin and evolution
Ceres is possibly a surviving protoplanet (planetary embryo), which formed 4.57 billion years ago in the asteroid belt. Although the majority of inner Solar System protoplanets (including all lunar- to Mars-sized bodies) either merged with other protoplanets to form terrestrial planets or were ejected from the Solar System by Jupiter, Ceres is thought to have survived relatively intact. An alternative theory proposes that Ceres formed in the Kuiper belt and later migrated to the asteroid belt. The discovery of ammonia salts in Occator crater supports an origin in the outer Solar System. However, the presence of ammonia ices can be attributed to impacts by comets, nevertheless, ammonia salts are more likely to be native to the surface.  Another possible protoplanet, Vesta, is less than half the size of Ceres; it suffered a major impact after solidifying, losing ~1% of its mass.
The geological evolution of Ceres was dependent on the heat sources available during and after its formation: friction from planetesimal accretion, and decay of various radionuclides (possibly including short-lived extinct radionuclides such as aluminium-26). These are thought to have been sufficient to allow Ceres to differentiate into a rocky core and icy mantle soon after its formation. This process may have caused resurfacing by water volcanism and tectonics, erasing older geological features. Ceres's relatively warm surface temperature implies that any of the resulting ice on its surface would have gradually sublimated, leaving behind various hydrated minerals like clay minerals and carbonates.
Today, Ceres has become considerably less geologically active, with a surface sculpted chiefly by impacts; nevertheless, evidence from Dawn reveals that internal processes have continued to sculpt Ceres's surface to a significant extent, in stark contrast to Vesta and of previous expectations that Ceres would have become geologically dead early in its history due to its small size. The presence of significant amounts of water ice in its crust and evidence of recent geological resurfacing, raises the possibility that Ceres has a layer of liquid water in its interior. This hypothetical layer is often called an ocean. If such a layer of liquid water exists, it is hypothesized to be located between the rocky core and ice mantle like that of the theorized ocean on Europa. The existence of an ocean is more likely if solutes (i.e. salts), ammonia, sulfuric acid or other antifreeze compounds are dissolved in the water.
Although not as actively discussed as a potential home for microbial extraterrestrial life as Mars, Europa, Enceladus, or Titan, there is evidence that Ceres' icy mantle was once a watery subterranean ocean, and that has led to speculations that life could have existed there, and that hypothesized ejecta bearing microorganisms could have come from Ceres to Earth. The remote detection of organic compounds and the presence of water with 20% carbon by mass in its near surface, could provide conditions favorable to organic chemistry.
Observation and exploration
When in opposition near its perihelion, Ceres can reach an apparent magnitude of +6.7. This is generally regarded as too dim to be visible to the naked eye, but under ideal viewing conditions, keen eyes with 20/20 vision may be able to see it. The only other asteroids that can reach a similarly bright magnitude are 4 Vesta and, when in rare oppositions near their perihelions, 2 Pallas and 7 Iris. When in conjunction, Ceres has a magnitude of around +9.3, which corresponds to the faintest objects visible with 10×50 binoculars; thus it can be seen with such binoculars in a naturally dark and clear night sky around new moon.
Some notable observations and milestones for Ceres include the following:
- 1984 November 13: An occultation of a star by Ceres observed in Mexico, Florida and across the Caribbean.
- 1995 June 25: Ultraviolet Hubble Space Telescope images with 50-kilometer resolution.
- 2002: Infrared images with 30-km resolution taken with the Keck telescope using adaptive optics.
- 2003 and 2004: Visible light images with 30-km resolution (the best prior to the Dawn mission) taken using Hubble.
- 2012 December 22: Ceres occulted the star TYC 1865-00446-1 over parts of Japan, Russia, and China. Ceres' brightness was magnitude 6.9 and the star, 12.2.
- 2014: Ceres was found to have an tenuous atmosphere (exosphere) of water vapor, confirmed by the Herschel space telescope.
- 2015: The NASA Dawn spacecraft approached and orbited Ceres, sending detailed images and scientific data back to Earth.
In 1981, a proposal for an asteroid mission was submitted to the European Space Agency (ESA). Named the Asteroidal Gravity Optical and Radar Analysis (AGORA), this spacecraft was to launch some time in 1990–1994 and perform two flybys of large asteroids. The preferred target for this mission was Vesta. AGORA would reach the asteroid belt either by a gravitational slingshot trajectory past Mars or by means of a small ion engine. However, the proposal was refused by ESA. A joint NASA–ESA asteroid mission was then drawn up for a Multiple Asteroid Orbiter with Solar Electric Propulsion (MAOSEP), with one of the mission profiles including an orbit of Vesta. NASA indicated they were not interested in an asteroid mission. Instead, ESA set up a technological study of a spacecraft with an ion drive. Other missions to the asteroid belt were proposed in the 1980s by France, Germany, Italy, and the United States, but none were approved. Exploration of Ceres by fly-by and impacting penetrator was the second main target of the second plan of the multiaimed Soviet Vesta mission, developed in cooperation with European countries for realisation in 1991–1994 but canceled due to the Soviet Union disbanding.
In the early 1990s, NASA initiated the Discovery Program, which was intended to be a series of low-cost scientific missions. In 1996, the program's study team recommended as a high priority a mission to explore the asteroid belt using a spacecraft with an ion engine. Funding for this program remained problematic for several years, but by 2004 the Dawn vehicle had passed its critical design review.
It was launched on 27 September 2007, as the space mission to make the first visits to both Vesta and Ceres. On 3 May 2011, Dawn acquired its first targeting image 1.2 million kilometers from Vesta. After orbiting Vesta for 13 months, Dawn used its ion engine to depart for Ceres, with gravitational capture occurring on 6 March 2015 at a separation of 61,000 km, four months prior to the New Horizons flyby of Pluto.
Dawn's mission profile called for it to study Ceres from a series of circular polar orbits at successively lower altitudes. It entered its first observational orbit ("RC3") around Ceres at an altitude of 13,500 km on 23 April 2015, staying for only approximately one orbit (fifteen days). The spacecraft subsequently reduced its orbital distance to 4,400 km for its second observational orbit ("survey") for three weeks, then down to 1,470 km ("HAMO;" high altitude mapping orbit) for two months and then down to its final orbit at 375 km ("LAMO;" low altitude mapping orbit) for at least three months. The spacecraft instrumentation includes a framing camera, a visual and infrared spectrometer, and a gamma-ray and neutron detector. These instruments examined Ceres' shape and elemental composition. On 13 January 2015, Dawn took the first images of Ceres at near-Hubble resolution, revealing impact craters and a small high-albedo spot on the surface, near the same location as that observed previously. Additional imaging sessions, at increasingly better resolution took place on 25 January 4, 12, 19, and 25 February 1 March, and 10 and 15 April.
Dawn's arrival in a stable orbit around Ceres was delayed after, close to reaching Ceres, it was hit by a cosmic ray, making it take another, longer route around Ceres in back, instead of a direct spiral towards it.
15 km (10 mi) of elevation separate the lowest crater floors (indigo) from the highest peaks (white).
Map of quadrangles
The following imagemap of the dwarf planet Ceres is divided into 15 quadrangles. They are named after the first craters whose names the IAU approved in July 2015. The map image(s) were taken by the Dawn space probe.
|RC3||1st||23 April 2015 – 9 May 2015||13,500 km (8,400 mi)||15 days||1.3||24×|
|Survey||2nd||6 June 2015 – 30 June 2015||4,400 km (2,700 mi)||3.1 days||0.41||73×|
|HAMO||3rd||17 August 2015 – 23 October 2015||1,450 km (900 mi)||19 hours||0.14 (140 m)||217×|
|LAMO/XMO1||4th||16 December 2015 – 2 September 2016||375 km (233 mi)||5.5 hours||0.035 (35 m)||850×|
|XMO2||5th||5 October 2016 – 4 November 2016||1,480 km (920 mi)||19 hours||0.14 (140 m)||217×|||
|XMO3||6th||5 December 2016 – 22 February 2018||7,520–9,350 km
|≈8 days||0.9 (est)||34× (est)|||
|XMO4||7th||22 April 2017 – 22 June 2017||13,830–52,800 km
|XMO5||8th||30 June 2017 – 16 April 2018||4,400–39,100 km
|XMO6||9th||14 May 2018 – 31 May 2018||440–4,700 km
|XMO7 (FINAL)||10th||6 June 2018 – present||35–4,000 km
17 August 2015: Dawn
3rd Map Orbit - HAMO
1,470 km (910 mi)
10 December 2015: Dawn
4th Map Orbit - LAMOa
385 km (239 mi)
10 December 2015: Dawn
4th Map Orbit - LAMOb
385 km (239 mi)
4 May 2015; Dawn
13,600 km (8,500 mi)
- Ceres (dwarf planet) in fiction
- Former classification of planets
- List of exceptional asteroids
- List of geological features on Ceres
- List of Solar System objects by size
- Mining of Ceres
- This image was taken by the Dawn spacecraft on 2 May 2015, during a "rotation characterization" orbit, 13,642 kilometres (8,477 mi) above the surface of Ceres. Visible at center and center right are two bright spots, a phenomenon common on Ceres, in Oxo and Haulani craters respectively. Ahuna Mons is also visible in the image as a noticeable, bluff hill, seen just right of bottom.
- The value of 0.37 is the mean moment of inertia, which is thought to better represent Ceres' interior structure than the polar moment of inertia (0.39), due to the high polar flattening.
- Due to its eccentric orbit, the dwarf planet Pluto was also within the orbit of Neptune from 1979 to 1999, and will be again from approximately 2227 to 2247.
- All other languages but one use a variant of Ceres/Cerere: Russian Tserera, Persian Seres, Japanese Keresu. The exception is Chinese, which uses 'grain-god(dess) star' (穀神星 gǔshénxīng). Note that this is unlike the goddess Ceres, where Chinese does use the Latin name (刻瑞斯 kèruìsī).
- In 1807 Klaproth tried to change the name to the more etymologically justified "cererium", but it did not catch on.
- This emission rate is modest compared to those calculated for the tidally driven plumes of Enceladus (a smaller body) and Europa (a larger body), 200 kg/s and 7000 kg/s, respectively.
- Schmadel, Lutz (2003). Dictionary of minor planet names (5th ed.). Germany: Springer. p. 15. ISBN 978-3-540-00238-3.
- Simpson, D. P. (1979). Cassell's Latin Dictionary (5th ed.). London: Cassell Ltd. p. 883. ISBN 978-0-304-52257-6.
- "The MeanPlane (Invariable plane) of the Solar System passing through the barycenter". 3 April 2009. Archived from the original on 14 May 2009. Retrieved 10 April 2009. (produced with Solex 10 Archived 29 April 2009 at WebCite written by Aldo Vitagliano; see also Invariable plane)
- "1 Ceres". JPL Small-Body Database Browser. Archived from the original on 4 August 2012. Retrieved 8 January 2015.
- "AstDyS-2 Ceres Synthetic Proper Orbital Elements". Department of Mathematics, University of Pisa, Italy. Archived from the original on 5 October 2011. Retrieved 1 October 2011.
- "05. Dawn Explores Ceres Results from the Survey Orbit" (PDF). Archived from the original (PDF) on 5 September 2015.
- Calculated based on the known parameters
- "DPS 2015: First reconnaissance of Ceres by Dawn".
- Park, R. S.; Konopliv, A. S.; Bills, B. G.; Rambaux, N.; Castillo-Rogez, J. C.; Raymond, C. A.; Vaughan, A. T.; Ermakov, A. I.; Zuber, M. T.; Fu, R. R.; Toplis, M. J.; Russell, C. T.; Nathues, A.; Preusker, F. (3 August 2016). "A partially differentiated interior for (1) Ceres deduced from its gravity field and shape". Nature. 537 (7621): 515–517. Bibcode:2016Natur.537..515P. doi:10.1038/nature18955. PMID 27487219.
- Chamberlain, Matthew A.; Sykes, Mark V.; Esquerdo, Gilbert A. (2007). "Ceres lightcurve analysis – Period determination". Icarus. 188 (2): 451–456. Bibcode:2007Icar..188..451C. doi:10.1016/j.icarus.2006.11.025.CS1 maint: Multiple names: authors list (link)
- "Asteroid Ceres P_constants (PcK) SPICE kernel file". Retrieved 5 November 2015.
- Konopliv, A.S.; Park, R.S.; Vaughan, A.T.; Bills, B.G.; Asmar, S.W.; Ermakov, A.I.; Rambaux, N.; Raymond, C.A.; Castillo-Rogez, J.C.; Russell, C.T.; Smith, D.E.; Zuber, M.T. (2018). "The Ceres gravity field, spin pole, rotation period and orbit from the Dawn radiometric tracking and optical data". Icarus. 299: 411–429. Bibcode:2018Icar..299..411K. doi:10.1016/j.icarus.2017.08.005.
- Li, Jian-Yang; McFadden, Lucy A.; Parker, Joel Wm. (2006). "Photometric analysis of 1 Ceres and surface mapping from HST observations". Icarus. 182 (1): 143–160. Bibcode:2006Icar..182..143L. doi:10.1016/j.icarus.2005.12.012.CS1 maint: Multiple names: authors list (link)
- Rivkin, A. S.; Volquardsen, E. L.; Clark, B. E. (2006). "The surface composition of Ceres: Discovery of carbonates and iron-rich clays" (PDF). Icarus. 185 (2): 563–567. Bibcode:2006Icar..185..563R. doi:10.1016/j.icarus.2006.08.022. Retrieved 8 December 2007.CS1 maint: Multiple names: authors list (link)
- Menzel, Donald H.; Pasachoff, Jay M. (1983). A Field Guide to the Stars and Planets (2nd ed.). Boston: Houghton Mifflin. p. 391. ISBN 978-0-395-34835-2.
- APmag and AngSize generated with Horizons(Ephemeris: Observer Table: Quantities = 9,13,20,29) Archived 5 October 2011 at WebCite
- Angelo, Joseph A., Jr (2006). Encyclopedia of Space and Astronomy. New York: Infobase. p. 122. ISBN 978-0-8160-5330-8.CS1 maint: Multiple names: authors list (link)
- Saint-Pé, O.; Combes, N.; Rigaut F. (1993). "Ceres surface properties by high-resolution imaging from Earth". Icarus. 105 (2): 271–281. Bibcode:1993Icar..105..271S. doi:10.1006/icar.1993.1125.CS1 maint: Multiple names: authors list (link)
- "Ceres". Dictionary.com. Random House, Inc. Archived from the original on 5 October 2011. Retrieved 26 September 2007.
- Stankiewicz, Rick (20 February 2015). "A visit to the asteroid belt". Peterborough Examiner. Retrieved 29 May 2015.
- Williams, Matt (23 August 2015). "What is the Asteroid Belt?". Universe Today. Retrieved 30 January 2016.
- "Dwarf Planet 1 Ceres Information". TheSkyLive.com. Retrieved 26 November 2017.
- "Ceres". Solar System Exploration: NASA Science. Retrieved 20 October 2018.
- McCord, T. B.; Sotin, C. (21 May 2005). "Ceres: Evolution and current state". Journal of Geophysical Research: Planets. 110 (E5): E05009. Bibcode:2005JGRE..110.5009M. doi:10.1029/2004JE002244.
- O'Brien, D. P.; Travis, B. J.; Feldman, W. C.; Sykes, M. V.; Schenk, P. M.; Marchi, S.; Russell, C. T.; Raymond, C. A. (March 2015). "The Potential for Volcanism on Ceres due to Crustal Thickening and Pressurization of a Subsurface Ocean" (PDF). 46th Lunar and Planetary Science Conference. p. 2831. Retrieved 1 March 2015.
- Tony Phillips, ed. (22 January 2014). "Water Detected on Dwarf Planet Ceres". Science@NASA. NASA.
- Landau, Elizabeth; Brown, Dwayne (6 March 2015). "NASA Spacecraft Becomes First to Orbit a Dwarf Planet". Jet Propulsion Laboratory. Retrieved 6 March 2015.
- "Dawn Spacecraft Begins Approach to Dwarf Planet Ceres". NASA. Retrieved 29 December 2014.
- Rayman, Marc (6 March 2015). "Dawn Journal: Ceres Orbit Insertion!". The Planetary Society. Retrieved 6 March 2015.
- Plait, Phil (11 May 2015). "The Bright Spots of Ceres Spin Into View". Slate. Retrieved 30 May 2015.
- O'Neill, I. (25 February 2015). "Ceres' Mystery Bright Dots May Have Volcanic Origin". Discovery Inc. Retrieved 1 March 2015.
- Landau, E. (25 February 2015). "'Bright Spot' on Ceres Has Dimmer Companion". Jet Propulsion Laboratory. Archived from the original on 26 February 2015. Retrieved 25 February 2015.
- Lakdawalla, E. (26 February 2015). "At last, Ceres is a geological world". The Planetary Society. Retrieved 26 February 2015.
- "LPSC 2015: First results from Dawn at Ceres: provisional place names and possible plumes". The Planetary Society.
- Atkinson, Nancy (3 March 2015). "Bright Spots on Ceres Likely Ice, Not Cryovolcanoes". Universe Today. Retrieved 4 March 2015.
- Sundermier, Ali. "NASA just found an ice volcano on Ceres that's half the size of Everest". ScienceAlert. Retrieved 5 September 2016.
- Ruesch, O.; Platz, T.; Schenk, P.; McFadden, L. A.; Castillo-Rogez, J. C.; Quick, L. C.; Byrne, S.; Preusker, F.; O’Brien, D. P. (2 September 2016). "Cryovolcanism on Ceres". Science. 353 (6303): aaf4286. Bibcode:2016Sci...353.4286R. doi:10.1126/science.aaf4286. ISSN 0036-8075. PMID 27701087.
- "Ceres RC3 Animation". Jet Propulsion Laboratory. 11 May 2015. Retrieved 31 July 2015.
- Landau, Elizabeth (9 December 2015). "New Clues to Ceres' Bright Spots and Origins". Jet Propulsion Laboratory. Retrieved 10 December 2015.
- Landau, Elizabeth; Greicius, Tony (29 June 2016). "Recent Hydrothermal Activity May Explain Ceres' Brightest Area". NASA. Retrieved 30 June 2016.
- Lewin, Sarah (29 June 2016). "Mistaken Identity: Ceres Mysterious Bright Spots Aren't Epsom Salt After All". Space.com. Retrieved 30 June 2016.
- De Sanctis, M. C.; et al. (29 June 2016). "Bright carbonate deposits as evidence of aqueous alteration on (1) Ceres". Nature. 536 (7614): 54–57. Bibcode:2016Natur.536...54D. doi:10.1038/nature18290. PMID 27362221.
- Landau, Elizabeth; McCartney, Gretchen (24 July 2018). "What Looks Like Ceres on Earth?". NASA. Retrieved 25 July 2018.
- Rayman, Marc (13 June 2018). "Dawn - Mission Status". Jet Propulsion Laboratory. Retrieved 16 June 2018.
- Clark, Stephen (15 June 2018). "Dawn spacecraft flying low over Ceres". SpaceFlightNow.com. Retrieved 16 June 2018.
- "Dawn data from Ceres publicly released: Finally, color global portraits!". The Planetary Society. Retrieved 9 November 2015.
- "Dawn discovers evidence for organic material on Ceres (Update)". Phys.org. 16 February 2017. Retrieved 17 February 2017.
- Combe, Jean-Philippe; Singh, Sandeep; Johnson, Katherine E.; McCord, Thomas B.; De Sanctis, Maria Cristina; Ammannito, Eleonora; Carrozzo, Filippo Giacomo; Ciarniello, Mauro; Frigeri, Alessandro; Raponi, Andrea; Tosi, Federico; Zambon, Francesca; Scully, Jennifer E.C.; Raymond, Carol A.; Russell, Christopher T. (2019). "The surface composition of Ceres' Ezinu quadrangle analyzed by the Dawn mission". Icarus. 318: 124–146. Bibcode:2019Icar..318..124C. doi:10.1016/j.icarus.2017.12.039.
- Hoskin, Michael (26 June 1992). "Bode's Law and the Discovery of Ceres". Observatorio Astronomico di Palermo "Giuseppe S. Vaiana". Archived from the original on 18 January 2010. Retrieved 5 July 2007.
- Hogg, Helen Sawyer (1948). "The Titius-Bode Law and the Discovery of Ceres". Journal of the Royal Astronomical Society of Canada. 242: 241–246. Bibcode:1948JRASC..42..241S.
- Hoskin, Michael (1999). The Cambridge Concise History of Astronomy. Cambridge University press. pp. 160–161. ISBN 978-0-521-57600-0.
- Landau, Elizabeth (26 January 2016). "Ceres: Keeping Well-Guarded Secrets for 215 Years". NASA. Retrieved 26 January 2016.
- Forbes, Eric G. (1971). "Gauss and the Discovery of Ceres". Journal for the History of Astronomy. 2 (3): 195–199. Bibcode:1971JHA.....2..195F. doi:10.1177/002182867100200305.
- Cunningham, Clifford J. (2001). The first asteroid: Ceres, 1801–2001. Star Lab Press. ISBN 978-0-9708162-1-4.
- Hilton, James L. "Asteroid Masses and Densities" (PDF). U.S. Naval Observatory. Retrieved 23 June 2008.
- Hughes, D. W. (1994). "The Historical Unravelling of the Diameters of the First Four Asteroids". R.A.S. Quarterly Journal. 35 (3): 331. Bibcode:1994QJRAS..35..331H. (Page 335)
- Foderà Serio, G.; Manara, A.; Sicoli, P. (2002). "Giuseppe Piazzi and the Discovery of Ceres" (PDF). In W. F. Bottke Jr.; A. Cellino; P. Paolicchi; R. P. Binzel (eds.). Asteroids III. Tucson, Arizona: University of Arizona Press. pp. 17–24. Retrieved 25 June 2009.
- Rüpke, Jörg (2011). A Companion to Roman Religion. John Wiley and Sons. pp. 90–. ISBN 978-1-4443-4131-7.
- Unicode value U+26B3
- Gould, B. A. (1852). "On the symbolic notation of the asteroids". Astronomical Journal. 2 (34): 80. Bibcode:1852AJ......2...80G. doi:10.1086/100212.
- "Cerium: historical information". Adaptive Optics. Retrieved 27 April 2007.
- "Cerium". Oxford English Dictionary (3rd ed.). Oxford University Press. September 2005. (Subscription or UK public library membership required.)
- "Amalgamator Features 2003: 200 Years Ago". 30 October 2003. Archived from the original on 7 February 2006. Retrieved 21 August 2006.
- Hilton, James L. (17 September 2001). "When Did the Asteroids Become Minor Planets?". Archived from the original on 18 January 2010. Retrieved 16 August 2006.
- Herschel, William (6 May 1802). "Observations on the two lately discovered celestial Bodies". Philosophical Transactions of the Royal Society of London. 92: 213–232. Bibcode:1802RSPT...92..213H. doi:10.1098/rstl.1802.0010. JSTOR 107120.
- Battersby, Stephen (16 August 2006). "Planet debate: Proposed new definitions". New Scientist. Archived from the original on 5 October 2011. Retrieved 27 April 2007.
- Connor, Steve (16 August 2006). "Solar system to welcome three new planets". NZ Herald. Archived from the original on 5 October 2011. Retrieved 27 April 2007.
- Gingerich, Owen; et al. (16 August 2006). "The IAU draft definition of "Planet" and "Plutons"". IAU. Archived from the original on 5 October 2011. Retrieved 27 April 2007.
- "The IAU Draft Definition of Planets And Plutons". SpaceDaily. 16 August 2006. Archived from the original on 18 January 2010. Retrieved 27 April 2007.
- Gaherty, Geoff; "How to Spot Giant Asteroid Vesta in Night Sky This Week", 3 August 2011 How to Spot Giant Asteroid Vesta in Night Sky This Week | Asteroid Vesta Skywatching Tips | Amateur Astronomy, Asteroids & Comets | Space.com Archived 5 October 2011 at WebCite
- "Question and answers 2". IAU. Archived from the original on 5 October 2011. Retrieved 31 January 2008.
- Spahr, T. B. (7 September 2006). "MPEC 2006-R19: EDITORIAL NOTICE". Minor Planet Center. Archived from the original on 5 October 2011. Retrieved 31 January 2008.
the numbering of "dwarf planets" does not preclude their having dual designations in possible separate catalogues of such bodies.
- Lang, Kenneth (2011). The Cambridge Guide to the Solar System. Cambridge University Press. pp. 372, 442. ISBN 9781139494175.
- NASA/JPL, Dawn Views Vesta, 2 August 2011 Archived 5 October 2011 at WebCite ("Dawn will orbit two of the largest asteroids in the Main Belt").
- de Pater; Lissauer (2010). Planetary Sciences (2nd ed.). Cambridge University Press. ISBN 978-0-521-85371-2.
- Mann, Ingrid; Nakamura, Akiko; Mukai, Tadashi (2009). Small bodies in planetary systems. Lecture Notes in Physics. 758. Springer-Verlag. ISBN 978-3-540-76934-7.
- Cellino, A.; et al. (2002). "Spectroscopic Properties of Asteroid Families" (PDF). Asteroids III. University of Arizona Press. pp. 633–643 (Table on p. 636). Bibcode:2002aste.book..633C.
- Kelley, M. S.; Gaffey, M. J. (1996). "A Genetic Study of the Ceres (Williams #67) Asteroid Family". Bulletin of the American Astronomical Society. 28: 1097. Bibcode:1996DPS....28.1009K.
- Kovačević, A. B. (2011). "Determination of the mass of Ceres based on the most gravitationally efficient close encounters". Monthly Notices of the Royal Astronomical Society. 419 (3): 2725–2736. arXiv:1109.6455. Bibcode:2012MNRAS.419.2725K. doi:10.1111/j.1365-2966.2011.19919.x.
- Christou, A. A. (2000). "Co-orbital objects in the main asteroid belt". Astronomy and Astrophysics. 356: L71–L74. Bibcode:2000A&A...356L..71C.
- Christou, A. A.; Wiegert, P. (January 2012). "A population of Main Belt Asteroids co-orbiting with Ceres and Vesta". Icarus. 217 (1): 27–42. arXiv:1110.4810. Bibcode:2012Icar..217...27C. doi:10.1016/j.icarus.2011.10.016. ISSN 0019-1035.
- "Solex numbers generated by Solex". Archived from the original on 29 April 2009. Retrieved 3 March 2009.
- Williams, David R. (2004). "Asteroid Fact Sheet". Archived from the original on 18 January 2010. Retrieved 14 January 2008.
- Schorghofer, N.; Mazarico, E.; Platz, T.; Preusker, F.; Schröder, S. E.; Raymond, C. A.; Russell, C. T. (6 July 2016). "The permanently shadowed regions of dwarf planet Ceres". Geophysical Research Letters. 43 (13): 6783–6789. Bibcode:2016GeoRL..43.6783S. doi:10.1002/2016GL069368.
- Rayman, Marc D. (28 May 2015). "Dawn Journal, May 28, 2015". Jet Propulsion Laboratory. Archived from the original on 30 May 2015. Retrieved 29 May 2015.
- Pitjeva, E. V. (2005). "High-Precision Ephemerides of Planets—EPM and Determination of Some Astronomical Constants". Solar System Research. 39 (3): 176–186. Bibcode:2005SoSyR..39..176P. doi:10.1007/s11208-005-0033-2.
- Thomas, P. C.; Parker, J. Wm.; McFadden, L. A.; et al. (2005). "Differentiation of the asteroid Ceres as revealed by its shape". Nature. 437 (7056): 224–226. Bibcode:2005Natur.437..224T. doi:10.1038/nature03938. PMID 16148926.CS1 maint: Multiple names: authors list (link)
- Approximately forty percent that of Australia, a third the size of the US or Canada, 12× that of the UK
- Thomas, P. C. (July 2010). "Sizes, shapes, and derived properties of the saturnian satellites after the Cassini nominal mission" (PDF). Icarus. 208 (1): 395–401. Bibcode:2010Icar..208..395T. doi:10.1016/j.icarus.2010.01.025.
- Neumann, W.; Breuer, D.; Spohn, T. (2 December 2015). "Modelling the internal structure of Ceres: Coupling of accretion with compaction by creep and implications for the water-rock differentiation" (PDF). Astronomy & Astrophysics. 584: A117. Bibcode:2015A&A...584A.117N. doi:10.1051/0004-6361/201527083.
- Bhatia, G.K.; Sahijpal, S. (2017). "Thermal evolution of trans-Neptunian objects, icy satellites, and minor icy planets in the early solar system". Meteoritics & Planetary Science. 52 (12): 2470–2490. Bibcode:2017M&PS...52.2470B. doi:10.1111/maps.12952.
- "Where is the Ice on Ceres? New NASA Dawn Findings". NASA. 15 December 2016. Retrieved 19 December 2016.
- Parker, J. W.; Stern, Alan S.; Thomas Peter C.; et al. (2002). "Analysis of the first disk-resolved images of Ceres from ultraviolet observations with the Hubble Space Telescope". The Astronomical Journal. 123 (1): 549–557. arXiv:astro-ph/0110258. Bibcode:2002AJ....123..549P. doi:10.1086/338093.CS1 maint: Multiple names: authors list (link)
- "Sulfur, Sulfur Dioxide, Graphitized Carbon Observed on Ceres". spaceref.com. 3 September 2016. Retrieved 8 September 2016.
- Carry, Benoit; et al. (2007). "Near-Infrared Mapping and Physical Properties of the Dwarf-Planet Ceres" (PDF). Astronomy & Astrophysics. 478 (1): 235–244. arXiv:0711.1152. Bibcode:2008A&A...478..235C. doi:10.1051/0004-6361:20078166. Archived from the original (PDF) on 30 May 2008.
- "Keck Adaptive Optics Images the Dwarf Planet Ceres". Adaptive Optics. 11 October 2006. Archived from the original on 18 January 2010. Retrieved 27 April 2007.
- "Largest Asteroid May Be 'Mini Planet' with Water Ice". HubbleSite. 7 September 2005. Archived from the original on 5 October 2011. Retrieved 16 August 2006.
- Arizona State University (26 July 2016). "The case of the missing craters". ScienceDaily. Retrieved 8 March 2017.
- Marchi, S.; Ermakov, A. I.; Raymond, C. A.; Fu, R. R.; O’Brien, D. P.; Bland, M. T.; Ammannito, E.; De Sanctis, M. C.; Bowling, T.; Schenk, P.; Scully, J. E. C.; Buczkowski, D. L.; Williams, D. A.; Hiesinger, H.; Russell, C. T. (26 July 2016). "The missing large impact craters on Ceres". Nature Communications. 7: 12257. Bibcode:2016NatCo...712257M. doi:10.1038/ncomms12257. PMC 4963536. PMID 27459197.
- "News – Ceres Spots Continue to Mystify in Latest Dawn Images". NASA/JPL.
- Steigerwald, Bill (2 September 2016). "NASA Discovers "Lonely Mountain" on Ceres Likely a Salty-Mud Cryovolcano". NASA. Retrieved 8 March 2017.
- "Ceres: The tiny world where volcanoes erupt ice". SpaceDaily. 5 September 2016. Retrieved 8 March 2017.
- Sori, Michael M.; Byrne, Shane; Bland, Michael T.; Bramson, Ali M.; Ermakov, Anton I.; Hamilton, Christopher W.; Otto, Katharina A.; Ruesch, Ottaviano; Russell, Christopher T. (2017). "The vanishing cryovolcanoes of Ceres". Geophysical Research Letters. 44 (3): 1243–1250. Bibcode:2017GeoRL..44.1243S. doi:10.1002/2016GL072319. hdl:10150/623032.
- "USGS: Ceres nomenclature" (PDF). Retrieved 16 July 2015.
- Rayman, Marc (8 April 2015). Now Appearing At a Dwarf Planet Near You: NASA's Dawn Mission to the Asteroid Belt (Speech). Silicon Valley Astronomy Lectures. Foothill College, Los Altos, CA. Retrieved 7 July 2018.
- Landau, Elizabeth (11 May 2015). "Ceres Animation Showcases Bright Spots". NASA. Retrieved 13 May 2015.
- Witze, Alexandra (21 July 2015). "Mystery haze appears above Ceres's bright spots". Nature News. doi:10.1038/nature.2015.18032. Retrieved 23 July 2015.
- Rivkin, Andrew (21 July 2015). "Dawn at Ceres: A haze in Occator crater?". The Planetary Society. Retrieved 8 March 2017.
- "Dawn Mission – News – Detail". NASA.
- Redd, Nola Taylor. "Water Ice on Ceres Boosts Hopes for Buried Ocean [Video]". Scientific American. Retrieved 7 April 2016.
- Preferential formation of sodium salts from frozen sodium-ammonium-chloride-carbonate brines – Implications for Ceres’ bright spots. Tuan H. Vu, Robert Hodyss, Paul V. Johnson, Mathieu Choukroun. Planetary and Space Science, Volume 141, July 2017, Pages 73-77
- McCord, Thomas B.; Zambon, Francesca (2019). "The surface composition of Ceres from the Dawn mission". Icarus. 318: 2–13. Bibcode:2019Icar..318....2M. doi:10.1016/j.icarus.2018.03.004.
- De Sanctis, M. C.; et al. (29 June 2016). "Bright carbonate deposits as evidence of aqueous alteration on (1) Ceres". Nature. 536 (7614): 54–57. Bibcode:2016Natur.536...54D. doi:10.1038/nature18290. PMID 27362221.
- Anderson, Paul Scott (27 December 2018). "What does Ceres' carbon mean?". Earth & Sky. Retrieved 27 December 2018.
- Team finds evidence for carbon-rich surface on Ceres. Southwest Research Institute. Published by PhysOrg. 10 December 2018.
- Marchi, S.; Raponi, A.; Prettyman, T. H.; De Sanctis, M. C.; Castillo-Rogez, J.; Raymond, C. A.; Ammannito, E.; Bowling, T.; Ciarniello, M.; Kaplan, H.; Palomba, E.; Russell, C. T.; Vinogradoff, V.; Yamashita, N. (2018). "An aqueously altered carbon-rich Ceres". Nature Astronomy. 3 (2): 140–145. Bibcode:2018NatAs.tmp..181M. doi:10.1038/s41550-018-0656-0.
- "PIA20348: Ahuna Mons Seen from LAMO". Jet Propulsion Lab. 7 March 2016. Retrieved 14 April 2016.
- "What's Inside Ceres? New Findings from Gravity Data". Jet Propulsion Laboratory.
- [https://solarsystem.nasa.gov/planets/dwarf-planets/ceres/in-depth/ Ceres: In Depth (NASA)
- M. Neveu and S. J. Desch (2016) 'Geochemistry, thermal evolution, and cryovolanism on Ceres with a muddy ice mantle'. 47th Lunar and Planetary Science Conference
- "Ceres takes life an ice volcano at a time". University of Arizona. 17 September 2018. Retrieved 22 April 2019.
- "PIA22660: Ceres' Internal Structure (Artist's Concept)". Photojournal. Jet Propulsion Laboratory. 14 August 2018. Retrieved 22 April 2019. This article incorporates text from this source, which is in the public domain.
- A'Hearn, Michael F.; Feldman, Paul D. (1992). "Water vaporization on Ceres". Icarus. 98 (1): 54–60. Bibcode:1992Icar...98...54A. doi:10.1016/0019-1035(92)90206-M.
- Ceres: The Smallest and Closest Dwarf Planet. Space.com 22 January 2014
- Dwarf Planet Ceres, Artist's Impression. 21 January 2014. NASA
- Jewitt, D; Chizmadia, L.; Grimm, R.; Prialnik, D (2007). "Water in the Small Bodies of the Solar System" (PDF). In Reipurth, B.; Jewitt, D.; Keil, K. (eds.). Protostars and Planets V. University of Arizona Press. pp. 863–878. ISBN 978-0-8165-2654-3.
- Küppers, M.; O'Rourke, L.; Bockelée-Morvan, D.; Zakharov, V.; Lee, S.; Von Allmen, P.; Carry, B.; Teyssier, D.; Marston, A.; Müller, T.; Crovisier, J.; Barucci, M. A.; Moreno, R. (23 January 2014). "Localized sources of water vapour on the dwarf planet (1) Ceres". Nature. 505 (7484): 525–527. Bibcode:2014Natur.505..525K. doi:10.1038/nature12918. ISSN 0028-0836. PMID 24451541.
- Campins, H.; Comfort, C. M. (23 January 2014). "Solar system: Evaporating asteroid". Nature. 505 (7484): 487–488. Bibcode:2014Natur.505..487C. doi:10.1038/505487a. PMID 24451536.
- Hansen, C. J.; Esposito, L.; Stewart, A. I.; Colwell, J.; Hendrix, A.; Pryor, W.; Shemansky, D.; West, R. (10 March 2006). "Enceladus' Water Vapor Plume". Science. 311 (5766): 1422–1425. Bibcode:2006Sci...311.1422H. doi:10.1126/science.1121254. PMID 16527971.
- Roth, L.; Saur, J.; Retherford, K. D.; Strobel, D. F.; Feldman, P. D.; McGrath, M. A.; Nimmo, F. (26 November 2013). "Transient Water Vapor at Europa's South Pole" (PDF). Science. 343 (6167): 171–174. Bibcode:2014Sci...343..171R. doi:10.1126/science.1247051. PMID 24336567. Retrieved 26 January 2014.
- Arizona State University (1 September 2016). "Ceres: The tiny world where volcanoes erupt ice". ScienceDaily. Retrieved 8 March 2017.
- Hiesinger, H.; Marchi, S.; Schmedemann, N.; Schenk, P.; Pasckert, J. H.; Neesemann, A.; OBrien, D. P.; Kneissl, T.; Ermakov, A. I.; Fu, R. R.; Bland, M. T.; Nathues, A.; Platz, T.; Williams, D. A.; Jaumann, R.; Castillo-Rogez, J. C.; Ruesch, O.; Schmidt, B.; Park, R. S.; Preusker, F.; Buczkowski, D. L.; Russell, C. T.; Raymond, C. A. (1 September 2016). "Cratering on Ceres: Implications for its crust and evolution". Science. 353 (6303): aaf4759. Bibcode:2016Sci...353.4759H. doi:10.1126/science.aaf4759. PMID 27701089.
- NASA/Jet Propulsion Laboratory (1 September 2016). "Ceres' geological activity, ice revealed in new research". ScienceDaily. Retrieved 8 March 2017.
- "Confirmed: Ceres Has a Transient Atmosphere - Universe Today". Universe Today. 6 April 2017. Retrieved 14 April 2017.
- Petit, Jean-Marc; Morbidelli, Alessandro (2001). "The Primordial Excitation and Clearing of the Asteroid Belt" (PDF). Icarus. 153 (2): 338–347. Bibcode:2001Icar..153..338P. doi:10.1006/icar.2001.6702. Retrieved 25 June 2009.
- Approximately a 10% chance of the asteroid belt acquiring a Ceres-mass KBO. McKinnon, William B.; (2008) "On the Possibility of Large KBOs Being Injected Into the Outer Asteroid Belt". American Astronomical Society, DPS meeting No. 40, #38.03 Bibcode: 2008DPS....40.3803M
- Greicius, Tony (29 June 2016). "Recent Hydrothermal Activity May Explain Ceres' Brightest Area". nasa.gov.
- Snodgrass, Colin; Agarwal, Jessica; Combi, Michael; Fitzsimmons, Alan; Guilbert-Lepoutre, Aurelie; Hsieh, Henry H.; Hui, Man-To; Jehin, Emmanuel; Kelley, Michael S. P. (14 November 2017). "The Main Belt Comets and ice in the Solar System" (PDF). The Astronomy and Astrophysics Review. 25 (1): 5. arXiv:1709.05549. Bibcode:2017A&ARv..25....5S. doi:10.1007/s00159-017-0104-7. ISSN 1432-0754.
- Thomas, Peter C.; Binzel, Richard P.; Gaffey, Michael J.; et al. (1997). "Impact Excavation on Asteroid 4 Vesta: Hubble Space Telescope Results". Science. 277 (5331): 1492–1495. Bibcode:1997Sci...277.1492T. doi:10.1126/science.277.5331.1492.CS1 maint: Multiple names: authors list (link)
- Wall, Mike (2 September 2016). "NASA's Dawn Mission Spies Ice Volcanoes on Ceres". Scientific American. Retrieved 8 March 2017.
- Castillo-Rogez, J. C.; McCord, T. B.; and Davis, A. G. (2007). "Ceres: evolution and present state" (PDF). Lunar and Planetary Science. XXXVIII: 2006–2007. Retrieved 25 June 2009.CS1 maint: Multiple names: authors list (link)
- Wall, Mike (27 July 2014). "Strange Bright Spots on Ceres Create Mini-Atmosphere on Dwarf Planet". Space.com. Retrieved 3 August 2015.
- Catling, David C. (2013). Astrobiology: A Very Short Introduction. Oxford: Oxford University Press. p. 99. ISBN 978-0-19-958645-5.
- Castillo-Rogez, J. C.; Conrad, P. G. (2010). Habitability Potential of Ceres, a Warm Icy Body in the Asteroid Belt (PDF). LPI Conference 2010. Lunar and Planetary Institute.
- Hand, Eric (20 February 2015). "Dawn probe to look for a habitable ocean on Ceres". Science. 347 (6224): 813–814. Bibcode:2015Sci...347..813H. doi:10.1126/science.347.6224.813. PMID 25700494.
- Houtkooper, Joop M.; "Glaciopanspermia: Seeding the Terrestrial Planets with Life?" Archived 22 July 2011 at the Wayback Machine Institute for Psychobiology and Behavioral Medicine, Justus-Liebig-University, Giessen, Germany
- O'Neill, Ian (5 March 2009). "Life on Ceres: Could the Dwarf Planet be the Root of Panspermia". Universe Today. Retrieved 30 January 2012.
- "SPHERE Maps the Surface of Ceres". Retrieved 8 September 2015.
- Martinez, Patrick (1994). The Observer's Guide to Astronomy. Cambridge University Press. p. 298.
- Millis, L. R.; Wasserman, L. H.; Franz, O. Z.; et al. (1987). "The size, shape, density, and albedo of Ceres from its occultation of BD+8°471". Icarus. 72 (3): 507–518. Bibcode:1987Icar...72..507M. doi:10.1016/0019-1035(87)90048-0. hdl:2060/19860021993.CS1 maint: Multiple names: authors list (link)
- "Observations reveal curiosities on the surface of asteroid Ceres". Archived from the original on 5 October 2011. Retrieved 16 August 2006.
- "Asteroid Occultation Updates". Asteroidoccultation.com. 22 December 2012. Archived from the original on 12 July 2012. Retrieved 20 August 2013.
- "Water Detected on Dwarf Planet Ceres". Science.nasa.gov. Retrieved 24 January 2014.
- Ulivi, Paolo; Harland, David (2008). Robotic Exploration of the Solar System: Hiatus and Renewal, 1983–1996. Springer Praxis Books in Space Exploration. Springer. pp. 117–125. ISBN 978-0-387-78904-0.
- Russell, C. T.; Capaccioni, F.; Coradini, A.; et al. (October 2007). "Dawn Mission to Vesta and Ceres" (PDF). Earth, Moon, and Planets. 101 (1–2): 65–91. Bibcode:2007EM&P..101...65R. doi:10.1007/s11038-007-9151-9. Retrieved 13 June 2011.CS1 maint: Multiple names: authors list (link)
- Cook, Jia-Rui C.; Brown, Dwayne C. (11 May 2011). "NASA's Dawn Captures First Image of Nearing Asteroid". NASA/JPL. Retrieved 14 May 2011.
- Schenk, P. (15 January 2015). "Year of the 'Dwarves': Ceres and Pluto Get Their Due". Planetary Society. Retrieved 10 February 2015.
- Rayman, Marc (1 December 2014). "Dawn Journal: Looking Ahead at Ceres". Planetary Society. Retrieved 2 March 2015.
- Rayman, Marc (3 March 2014). "Dawn Journal: Maneuvering Around Ceres". Planetary Society. Retrieved 6 March 2015.
- Rayman, Marc (30 April 2014). "Dawn Journal: Explaining Orbit Insertion". Planetary Society. Retrieved 6 March 2015.
- Rayman, Marc (30 June 2014). "Dawn Journal: HAMO at Ceres". Planetary Society. Retrieved 6 March 2015.
- Rayman, Marc (31 August 2014). "Dawn Journal: From HAMO to LAMO and Beyond". Planetary Society. Retrieved 6 March 2015.
- Russel, C. T.; Capaccioni, F.; Coradini, A.; et al. (2006). "Dawn Discovery mission to Vesta and Ceres: Present status". Advances in Space Research. 38 (9): 2043–2048. arXiv:1509.05683. Bibcode:2006AdSpR..38.2043R. doi:10.1016/j.asr.2004.12.041.CS1 maint: Multiple names: authors list (link)
- Rayman, Marc (30 January 2015). "Dawn Journal: Closing in on Ceres". Planetary Society. Retrieved 2 March 2015.
- "Dawn Operating Normally After Safe Mode Triggered". NASA/JPL. 16 September 2014. Archived from the original on 25 December 2014. Retrieved 18 March 2015.
- China's Deep-space Exploration to 2030 by Zou Yongliao Li Wei Ouyang Ziyuan Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing
- Landau, Elizabeth (28 July 2015). "New Names and Insights at Ceres". NASA. Retrieved 28 July 2015.
- Staff (17 July 2015). "First 17 Names Approved for Features on Ceres". USGS. Archived from the original on 6 August 2015. Retrieved 9 August 2015.
- Krummheuer, B. (25 February 2015). "Dawn: Two new glimpses of dwarf planet Ceres". Max Planck Institute for Solar System Research. Retrieved 26 February 2015.
- Rayman, Marc (25 February 2015). "Dawn Journal: Ceres' Deepening Mysteries". Planetary Society. Retrieved 25 February 2015.
- Rayman, Marc (31 March 2015). "Dawn Journal March 31 ". NASA / Jet Propulsion Laboratory. Archived from the original on 5 September 2015. Retrieved 9 September 2015.
- Rayman, Marc (30 July 2015). "Dawn Journal: Descent to HAMO". The Planetary Society. Retrieved 9 September 2015.
- "PIA21221: Dawn XMO2 Image 1". NASA / Jet Propulsion Laboratory. 7 November 2016. Retrieved 20 November 2016.
- "Dawn Mission Status Updates". NASA / Jet Propulsion Laboratory. 16 October 2015. Retrieved 17 October 2015.
- Rayman, Marc D. (28 November 2016). "Dawn Journal". NASA/JPL. Retrieved 8 March 2017.
- Rayman, Marc (2017). "2017 Mission Status Updates". NASA / Jet Propulsion Laboratory.
- Rayman, Marc (25 May 2018). "Dawn Journal: Getting Elliptical". The Planetary Society. Retrieved 5 June 2018.
- Rayman, Marc (20 March 2018). "Dear Vernal Dawnquinoxes". NASA. Retrieved 5 June 2018.
- Rayman, Marc (2018). "2018 Mission Status Archive". NASA / Jet Propulsion Laboratory.
- Kornfeld, Laurel (2 June 2018). "Dawn will enter lowest ever orbit around Ceres". Spaceflight Insider. Retrieved 5 June 2018.
- Rayman, Marc (29 April 2018). "Dear Isaac Newdawn, Charles Dawnwin, Albert Einsdawn and all other science enthusiasts". NASA. Retrieved 5 June 2018.
- Landau, Elizabeth; Dyches, Preston (8 June 2015). "Fly Over Ceres in New Video". NASA. Retrieved 9 June 2015.
|Wikimedia Commons has media related to Ceres (dwarf planet).|
- Ceres Trek – An integrated map browser of datasets and maps for 1 Ceres
- Destination Ceres:Breakfast at Dawn – NASA
- Dawn mission home page at JPL
- Simulation of the orbit of Ceres
- Google Ceres 3D, interactive map of the dwarf planet
- How Gauss determined the orbit of Ceres from keplersdiscovery.com
- Hilton, James L. (1999). "U.S. Naval Observatory Ephemerides of the Largest Asteroids". The Astronomical Journal. 117 (2): 1077–1086. Bibcode:1999AJ....117.1077H. doi:10.1086/300728.
- Animated reprojected colorized map of Ceres (22 February 2015)
- Rotating relief model of Ceres by Seán Doran (about 60% of a full rotation; starts with Occator midway above center)
- Ceres (dwarf planet) at AstDyS-2, Asteroids—Dynamic Site
- Ceres at the JPL Small-Body Database