Achmad Kevin Ihza: Ceres (dwarf planet)

Ceres (/ˈsɪəriːz/;^[18] minor-planet designation:1 Ceres) is the largest object in the asteroid belt that lies between the orbits of Mars andJupiter. Its diameter is approximately 945 kilometers (587 miles),^[6] making it the largest of the minor planets within the orbit ofNeptune. The 33rd-largest known body in theSolar System, it is the only one identified orbiting entirely within the orbit of Neptune that is a dwarf planet.^[19] Composed of rock and ice, Ceres is estimated to comprise 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. From Earth, the apparent magnitude of Ceres ranges from 6.7 to 9.3, and hence even at its brightest, it is too dim to be seen with the naked eye, except under extremely dark skies.

Ceres was the first asteroid discovered, byGiuseppe Piazzi at Palermo on 1 January 1801. It was originally considered a planet, but was reclassified as an asteroid in the 1850s when many other objects in similar orbits were discovered.

Ceres appears to be differentiated into arocky core and icy mantle, and may have a remnant internal ocean of liquid water under the layer of ice.^[20]^[21] The surface is probably a mixture of water ice and various hydratedminerals such as carbonates and clay. In January 2014, emissions of water vapor were detected from several regions of Ceres.^[22]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.^[23]^[24]^[25]Pictures with a resolution previously unattained were taken during imaging sessions starting in January 2015 as Dawnapproached Ceres, showing a cratered surface. Two distinct bright spots (or high-albedo features) inside a crater (different from the bright spots observed in earlierHubble images^[26]) were seen in a 19 February 2015 image, leading to speculation about a possible cryovolcanic origin^[27]^[28]^[29] or outgassing.^[30] 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,^[31]however on 2 September 2016, published alongside six other studies, NASA scientists released a paper in Science that claims that a massive ice volcano called Ahuna Mons is the strongest evidence yet for the existence of these mysterious ice volcanoes.^[32]^[33] On 11 May 2015, NASA released a higher-resolution image showing that, instead of one or two spots, there are actually several.^[34] 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 brinecontaining magnesium sulfate hexahydrite(MgSO₄·6H₂O); the spots were also found to be associated with ammonia-rich clays.^[35] In June 2016, near-infrared spectra of these bright areas were found to be consistent with a large amount of sodium carbonate, (Na
2CO
3), implying that recent geologic activity was probably involved in the creation of the bright spots.^[36]^[37]^[38]

In October 2015, NASA released a true color portrait of Ceres made by Dawn.^[39]

HistoryEdit

DiscoveryEdit

Piazzi's book"Della scoperta del nuovo pianeta Cerere Ferdinandea"outlining the discovery of Ceres, dedicated the new "planet" toFerdinand I of the Two Sicilies.

Johann Elert Bode, in 1772, first suggested that an undiscovered planet could exist between the orbits of Mars and Jupiter.^[40]Kepler had already noticed the gap between Mars and Jupiter in 1596.^[40] Bode based his idea on the Titius–Bode law—a now-discredited hypothesis Johann Daniel Titiusfirst proposed in 1766—observing that there was a regular pattern in the semi-major axes of the orbits of known planets, marred only by the large gap between Mars and Jupiter.^[40]^[41]The pattern predicted that the missing planet ought to have an orbit with a semi-major axis near 2.8 astronomical units (AU).^[41] William Herschel's discovery of Uranus in 1781^[40]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 theMonatliche Correspondenz, sent requests to twenty-four experienced astronomers (dubbed the "celestial police"), asking that they combine their efforts and begin a methodical search for the expected planet.^[40]^[41] Although they did not discover Ceres, they later found several largeasteroids.^[41]

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.^[42]^[43] 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".^[40] Instead of a star, Piazzi had found a moving star-like object, which he first thought was a comet.^[44] 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 Orianiof Milan and Bode of Berlin.^[45] 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".^[40] 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.^[44]

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.^[44] 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.^[44]

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 1811Johann Hieronymus Schröter overestimated it as 2,613 km.^[46]^[47]

NameEdit

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 ofSicily.^[40]^[44] "Ferdinandea", however, was not acceptable to other nations and was dropped. Ceres was called Hera for a short time in Germany.^[48] In Greece, it is called Demeter(Δήμητρα), after the Greek equivalent of the Roman Cerēs;^[c] in English, that name is used for the asteroid 1108 Demeter.

The regular adjectival forms of the name areCererian and Cererean,^[49] derived from theLatin genitive Cereris,^[2] 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 asickle, ⟨⚳⟩ ( ),^[50] 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⟩.^[44]^[51]

Cerium, a rare-earth element discovered in 1803, was named after Ceres.^[52]^[d] In the same year another element was also initially named after Ceres, but when cerium was named, its discoverer changed the name topalladium, after the second asteroid, 2 Pallas.^[54]

ClassificationEdit

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.^[40] 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.^[40]^[44]^[55]

Sizes of the first ten main-belt objects discovered profiled against theMoon. Ceres is far left (1).

As other objects were discovered in the neighborhood of Ceres, it was realized that Ceres represented the first of a new class of objects.^[40] In 1802, with the discovery of 2 Pallas, William Herschel coined the termasteroid ("star-like") for these bodies,^[55]writing that "they resemble small stars so much as hardly to be distinguished from them, even by very good telescopes".^[56] 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.^[55]

Ceres (bottom left), theMoon and Earth, shown to scale

Size comparison of Vesta, Ceres and Eros

The 2006 debate surrounding Pluto and what constitutes a planet led to Ceres being considered for reclassification as a planet.^[57]^[58] A proposal before theInternational Astronomical Union for thedefinition 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".^[59] Had this resolution been adopted, it would have made Ceres the fifth planet in order from the Sun.^[60] 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.^[13] 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",^[61] 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.^[62] The Minor Planet Center notes that such bodies may have dual designations.^[63] 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".^[64] NASA continues to refer to Ceres as an asteroid,^[65] as do various academic textbooks.^[66]^[67]

OrbitEdit

Proper (long-term mean) orbital elements compared to osculating (instant) orbital elements for Ceres:Element
typea
(in AU)e i Period
(in days)Proper ^[5]2.76710.1161989.6474351,681.60Osculating ^[4]
(Epoch 23 July 2010 )2.76530.07913810.5868211,679.66Difference0.00180.037060.9393861.94

Orbit of Ceres

Ceres follows an orbit between Mars and Jupiter, within the asteroid belt, with a period of 4.6 Earth years.^[4] The orbit is moderately inclined (i = 10.6° compared to 7° for Mercuryand 17° for Pluto) and moderately eccentric (e= 0.08 compared to 0.09 for Mars).^[4]

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 anasteroid family.^[68] 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.^[68] Ceres appears to be merely an interloper in the Gefion family, coincidentally having similar orbital elements but not a common origin.^[69]

ResonancesEdit

Ceres is in a near-1:1 mean-motion orbital resonance with Pallas (their proper orbital periods differ by 0.2%).^[70] 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.^[71] 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.^[72]

Transits of planets from CeresEdit

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.^[73]

Rotation and axial tiltEdit

The rotation period of Ceres (the Cererian day) is 9 hours and 4 minutes.^[74] It has a small axial tilt of 4°. This is nevertheless large 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.^[75]

GeologyEdit

Main article: Geology of Ceres

Ceres has a mass of 9.39×10²⁰ kg as determined from the Dawn spacecraft.^[76]With this mass Ceres comprises approximately a third of the estimated total 3.0 ± 0.2×10²¹ kg mass of the asteroid belt,^[77] which is in turn approximately 4% of the mass of the Moon. Ceres is massive enough to give it a nearly spherical,equilibrium shape.^[78] 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.^[79]

SurfaceEdit

Main article: List of geological features on Ceres

The surface composition of Ceres is broadly similar to that of C-type asteroids.^[13] 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) andcarbonate minerals (dolomite and siderite), which are common minerals in carbonaceous chondrite meteorites.^[13] The spectral features of carbonates and clay minerals are usually absent in the spectra of other C-type asteroids.^[13] Sometimes Ceres is classified as a G-type asteroid.^[80]

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.^[17] Ice is unstable at this temperature. 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.

VIR spectrometer mapping
(bw; true-color; IR) of Ceres.

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 Cerean conditions and would be expected to either escape quickly or settle in cold traps, and are evidently associated with areas with recent geological activity.^[81]

Observations prior to DawnEdit

HSTimages taken over a span of 2 hours and 20 minutes in 2004

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.^[80] This was thought to be a crater. Later near-infrared images with a higher resolution taken over a whole rotation with theKeck telescope using adaptive optics showed several bright and dark features moving with Ceres' rotation.^[82]^[83] 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.^[82]^[83] 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.^[12]^[84] One of these features corresponds to the "Piazzi" feature observed earlier.^[12]

These last observations indicated that the north pole of Ceres pointed in the direction ofright ascension 19 h 24 min (291°),declination +59°, in the constellation Draco, resulting in an axial tilt of approximately 3°.^[12]^[78] 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°.^[6]

Observations by DawnEdit

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Permanently shadowed regions capable of accumulating surface ice were identified in the northern hemisphere of Ceres using 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.^[85] An unexpectedly large number of Cererian craters have central pits, perhaps due to cryovolcanic processes, and many have central peaks.^[86]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.^[87]^[88] 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.^[89] 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%^[90] that are caused by a substance on the surface, possibly ice or salts, reflecting sunlight.^[91]^[92]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.^[92]^[93]In March 2016, Dawn found definitive evidence of water molecules on the surface of Ceres at Oxo crater.^[94]^[95] JPL states: "This water could be bound up in minerals or, alternatively, it could take the form of ice."

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.^[35] Another team thinks the salts are sodium carbonate.^[37]^[38]

Map of bright spots on Ceres (released 10 December 2015).

Bright spots on Ceres in visible and infrared:
"Spot 1" (top row) ("cooler" than surroundings);
"Spot 5" (bottom) ("similar in temperature" as surroundings) (April 2015)

"Bright Spot 5" in the crater Occator. Imaged by Dawn from 385 km (239 mi) (LAMO)

Ahuna Mons is an estimated 5 km (3 mi) high on its steepest side.^[96]Imaged by Dawn from 385 km (239 mi) in December 2015.

Internal structureEdit

Diagram showing a possible internal structure of Ceres

Ceres' oblateness is consistent with a differentiated body, a rocky core overlain with an icy mantle.^[78] This 100-kilometer-thick mantle (23%–28% of Ceres by mass; 50% byvolume)^[97] contains up to 200 million cubic kilometers of water, which would be more than the amount of fresh water on Earth.^[98]This result is supported by the observations made by the Keck telescope in 2002 and by evolutionary modeling.^[20]^[82] Also, some characteristics of its surface and history (such as its distance from the Sun, which weakened solar radiation enough to allow some fairly low-freezing-point components to be incorporated during its formation), point to the presence of volatile materials in the interior of Ceres.^[82] It has been suggested that a remnant layer of liquid water may have survived to the present under a layer of ice.^[20]^[21]

Shape and gravity field measurements byDawn confirm Ceres is a body in hydrostatic equilibrium with partial differentiation ^[8]^[99]and isostatic compensation, with a meanmoment of inertia of 0.37 (which is similar to that of Callisto at ~0.36).^[9] The densities of the core and outer layer are estimated to be 2.46–2.90 and 1.68–1.95 g/cm³, with the latter being about 70–190 km thick. Only partial dehydration of the core is expected. The high density of the outer layer (relative to water ice) reflects its enrichment in silicates and salts.^[9] 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.^[100] Modeling has suggested Ceres could have a small metallic core from partial differentiation of its rocky fraction.^[101]

AtmosphereEdit

There are indications that Ceres may have a tenuous water vapor atmosphere outgassing from water ice on the surface.^[102]^[103]^[104]

Surface water ice is unstable at distances less than 5 AU from the Sun,^[105] 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.^[82] Ultraviolet observations by theIUE spacecraft detected statistically significant amounts of hydroxide ions near Ceres' north pole, which is a product of water vapor dissociation by ultraviolet solar radiation.^[102]

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.^[106]^[107]^[e] 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 fromradiogenic internal heat^[106] or from pressurization of a subsurface ocean due to growth of an overlying layer of ice.^[21] 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;^[106] however, subsequent evidence from Dawn strongly suggests ongoing geologic activity could be at least partially responsible.^[110]

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.^[111]

Origin and evolution

Potential habitability

Observation and exploration

Maps

Gallery

Achmad Kevin Ihza

Selasa, 15 November 2016

Ceres (dwarf planet)

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