Dwarf planet - wikipedia Dwarf planet Not to be confused with minor planet. Five recognized dwarf planets Ceres ( 1801 ) Pluto ( 1930 ) Eris ( 2005 ) Makemake ( 2005 ) Haumea ( 2004 ) The five dwarf planets : Ceres as seen from the Dawn spacecraft. It is the only dwarf planet in the asteroid belt. Pluto as viewed by New Horizons space probe on July 13, 2015. Eris and its moon Dysnomia viewed by the Hubble Space Telescope. Makemake and its moon S / 2015 ( 136472 ) 1 viewed by the Hubble Space Telescope. NASA artist 's impression of Haumea. A dwarf planet is a planetary - mass object that is neither a true planet nor a natural satellite. That is, it is in direct orbit of a star, and is massive enough for its gravity to compress it into a hydrostatically equilibrious shape ( usually a spheroid ), but has not cleared the neighborhood of other material around its orbit. The term dwarf planet was adopted in 2006 as part of a three - way categorization of bodies orbiting the Sun, brought about by an increase in discoveries of objects farther away from the Sun than Neptune that rivaled Pluto in size, and finally precipitated by the discovery of an even more massive object, Eris. The exclusion of dwarf planets from the roster of planets by the IAU has been both praised and criticized ; it was said to be the `` right decision '' by astronomer Mike Brown, who discovered Eris and other new dwarf planets, but has been rejected by Alan Stern, who had coined the term dwarf planet in April 1991. As of July 2008 the International Astronomical Union ( IAU ) recognizes five dwarf planets : Ceres in the asteroid belt, and Pluto, Haumea, Makemake, and Eris in the outer Solar System. Brown criticizes this official recognition : `` A reasonable person might think that this means that there are five known objects in the solar system which fit the IAU definition of dwarf planet, but this reasonable person would be nowhere close to correct. '' Another hundred or so known objects in the Solar System are suspected to be dwarf planets. Estimates are that up to 200 dwarf planets will be identified when the entire region known as the Kuiper belt is explored, and that the number may exceed 10,000 when objects scattered outside the Kuiper belt are considered. Individual astronomers recognize several of these, and Brown maintains a list of hundreds of candidate objects, ranging from `` nearly certain '' to `` possible '' dwarf planets. As of 5 Feb 2018, Brown 's list includes 952 objects, identifying ten known trans - Neptunian objects -- the four accepted by the IAU plus 2007 OR, Quaoar, Sedna, Orcus, ( 307261 ) 2002 MS 4 and Salacia -- as `` near certain '', with another 27 `` highly likely. '' Stern states that there are more than a dozen known dwarf planets. Only two of these bodies, Ceres and Pluto, have been observed in enough detail to demonstrate that they actually fit the IAU 's definition. The IAU accepted Eris as a dwarf planet because it is more massive than Pluto. They subsequently decided that unnamed trans - Neptunian objects with an absolute magnitude brighter than + 1 ( and hence a diameter of ≥ 838 km assuming a geometric albedo of ≤ 1 ) are to be named under the assumption that they are dwarf planets. The classification of bodies in other planetary systems with the characteristics of dwarf planets has not been addressed. Contents 1 History of the concept 2 Name 3 Characteristics 3.1 Orbital dominance 3.2 Hydrostatic equilibrium 4 Dwarf planets and possible dwarf planets 4.1 Recognized 4.2 Proposed 5 Exploration 6 Contention 7 Planetary - mass moons 8 See also 9 Notes 10 References 11 External links History of the concept Main article : IAU definition of planet Pluto and its moon Charon 4 Vesta, one of the largest asteroids Starting in 1801, astronomers discovered Ceres and other bodies between Mars and Jupiter which were for decades considered to be planets. Between then and around 1851, when the number of planets had reached 23, astronomers started using the word asteroid for the smaller bodies and then stopped naming or classifying them as planets. With the discovery of Pluto in 1930, most astronomers considered the Solar System to have nine planets, along with thousands of significantly smaller bodies ( asteroids and comets ). For almost 50 years Pluto was thought to be larger than Mercury, but with the discovery in 1978 of Pluto 's moon Charon, it became possible to measure Pluto 's mass accurately and to determine that it was much smaller than initial estimates. It was roughly one - twentieth the mass of Mercury, which made Pluto by far the smallest planet. Although it was still more than ten times as massive as the largest object in the asteroid belt, Ceres, it had one - fifth the mass of Earth 's Moon. Furthermore, having some unusual characteristics, such as large orbital eccentricity and a high orbital inclination, it became evident that it was a different kind of body from any of the other planets. In the 1990s, astronomers began to find objects in the same region of space as Pluto ( now known as the Kuiper belt ), and some even farther away. Many of these shared several of Pluto 's key orbital characteristics, and Pluto started being seen as the largest member of a new class of objects, plutinos. This led some astronomers to stop referring to Pluto as a planet. Several terms, including subplanet and planetoid, started to be used for the bodies now known as dwarf planets. By 2005, three trans - Neptunian objects comparable in size to Pluto ( Quaoar, Sedna, and Eris ) had been reported. It became clear that either they would also have to be classified as planets, or Pluto would have to be reclassified. Astronomers were also confident that more objects as large as Pluto would be discovered, and the number of planets would start growing quickly if Pluto were to remain a planet. Eris ( then known as 2003 UB ) was discovered in January 2005 ; it was thought to be slightly larger than Pluto, and some reports informally referred to it as the tenth planet. As a consequence, the issue became a matter of intense debate during the IAU General Assembly in August 2006. The IAU 's initial draft proposal included Charon, Eris, and Ceres in the list of planets. After many astronomers objected to this proposal, an alternative was drawn up by the Uruguayan astronomers Julio Ángel Fernández and Gonzalo Tancredi : they proposed an intermediate category for objects large enough to be round but which had not cleared their orbits of planetesimals. Dropping Charon from the list, the new proposal also removed Pluto, Ceres, and Eris, because they have not cleared their orbits. The IAU 's final Resolution 5A preserved this three - category system for the celestial bodies orbiting the Sun. It reads : The IAU... resolves that planets and other bodies, except satellites, in our Solar System be defined into three distinct categories in the following way : ( 1 ) A planet is a celestial body that ( a ) is in orbit around the Sun, ( b ) has sufficient mass for its self - gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium ( nearly round ) shape, and ( c ) has cleared the neighbourhood around its orbit. ( 2 ) A `` dwarf planet '' is a celestial body that ( a ) is in orbit around the Sun, ( b ) has sufficient mass for its self - gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium ( nearly round ) shape, ( c ) has not cleared the neighbourhood around its orbit, and ( d ) is not a satellite. ( 3 ) All other objects, except satellites, orbiting the Sun shall be referred to collectively as `` Small Solar System Bodies. '' Footnotes : The eight planets are : Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, and Neptune. An IAU process will be established to assign borderline objects either dwarf planet or other status. These currently include most of the Solar System asteroids, most Trans - Neptunian Objects ( TNOs ), comets, and other small bodies. Although concerns were raised about the classification of planets orbiting other stars, the issue was not resolved ; it was proposed instead to decide this only when such objects start to be observed. Name Euler diagram showing the types of bodies in the Solar System ( except the Sun ). The term dwarf planet has itself been somewhat controversial, as it could imply that these bodies are planets, much as dwarf stars are stars. This is the conception of the Solar System that Stern promoted when he coined the phrase. The older word planetoid ( `` having the form of a planet '' ) has no such connotation, and is also used by astronomers for bodies that fit the IAU definition. Brown states that planetoid is `` a perfectly good word '' that has been used for these bodies for years, and that the use of the term dwarf planet for a non-planet is `` dumb '', but that it was motivated by an attempt by the IAU division III plenary session to reinstate Pluto as a planet in a second resolution. Indeed, the draft of Resolution 5A had called these median bodies planetoids, but the plenary session voted unanimously to change the name to dwarf planet. The second resolution, 5B, defined dwarf planets as a subtype of planet, as Stern had originally intended, distinguished from the other eight that were to be called `` classical planets ''. Under this arrangement, the twelve planets of the rejected proposal were to be preserved in a distinction between eight classical planets and four dwarf planets. Resolution 5B was defeated in the same session that 5A was passed. Because of the semantic inconsistency of a dwarf planet not being a planet due to the failure of Resolution 5B, alternative terms such as nanoplanet and subplanet were discussed, but there was no consensus among the CSBN to change it. In most languages equivalent terms have been created by translating dwarf planet more - or-less literally : French planète naine, Spanish planeta enano, German Zwergplanet, Russian karlikovaya planeta ( карликовая планета ), Arabic kaukab qazm ( كوكب قزم ), Chinese ǎixíngxīng ( 矮 行星 ), Korean waesohangseong ( 왜 소행성 ; 矮小 行星 ), but in Japanese they are called junwakusei ( 準 惑星 ) meaning `` subplanets '' or `` almost - planets ''. IAU Resolution 6a of 2006 recognizes Pluto as `` the prototype of a new category of trans - Neptunian objects ''. The name and precise nature of this category were not specified but left for the IAU to establish at a later date ; in the debate leading up to the resolution, the members of the category were variously referred to as plutons and plutonian objects but neither name was carried forward, perhaps due to objections from geologists that this would create confusion with their pluton. On June 11, 2008, the IAU Executive Committee announced a name, plutoid, and a definition : all trans - Neptunian dwarf planets are plutoids. The authority of that initial announcement has not been universally recognized : ``... in part because of an email miscommunication, the WG - PSN ( Working Group for Planetary System Nomenclature ) was not involved in choosing the word plutoid... In fact, a vote taken by the WG - PSN subsequent to the Executive Committee meeting has rejected the use of that specific term... '' Characteristics Planetary discriminants Body M / M Λ μ Π Mercury 0.055 1.95 × 10 9.1 × 10 1.3 × 10 Venus 0.815 1.66 × 10 1.35 × 10 9.5 × 10 Earth 1.53 × 10 1.7 × 10 8.1 × 10 Mars 0.107 9.42 × 10 1.8 × 10 5.4 × 10 Ceres 0.00015 8.32 × 10 0.33 4.0 × 10 Jupiter 317.7 1.30 × 10 6.25 × 10 4.0 × 10 Saturn 95.2 4.68 × 10 1.9 × 10 6.1 × 10 Uranus 14.5 3.85 × 10 2.9 × 10 4.2 × 10 Neptune 17.1 2.73 × 10 2.4 × 10 3.0 × 10 Pluto 0.0022 2.95 × 10 0.077 2.8 × 10 Eris 0.0028 2.13 × 10 0.10 2.0 × 10 Sedna 0.00022 3.64 × 10 < 0.07 1.6 × 10 Showing the planets and the largest known sub-planetary objects ( purple ) covering the orbital zones containing likely dwarf planets. All known possible dwarf planets have smaller discriminants than those shown for that zone. Mass in M, the unit of mass equal to that of Earth ( 5.97 × 10 kg ). Λ is the capacity to clear the neighbourhood ( greater than 1 for planets ) by Stern and Levison. Λ = k M a, where k = 0.0043 for units of Yg and AU, and a is the body 's semi-major axis. μ is Soter 's planetary discriminant ( greater than 100 for planets ). μ = M / m, where M is the mass of the body, and m is the aggregate mass of all the other bodies that share its orbital zone. Π is the capacity to clear the neighbourhood ( greater than 1 for planets ) by Margot. Π = k M a, where k = 807 for units of Earth masses and AU. Orbital dominance Main article : Clearing the neighbourhood Alan Stern and Harold F. Levison introduced a parameter Λ ( lambda ), expressing the likelihood of an encounter resulting in a given deflection of orbit. The value of this parameter in Stern 's model is proportional to the square of the mass and inversely proportional to the period. This value can be used to estimate the capacity of a body to clear the neighbourhood of its orbit, where Λ > 1 will eventually clear it. A gap of five orders of magnitude in Λ was found between the smallest terrestrial planets and the largest asteroids and Kuiper belt objects. Using this parameter, Steven Soter and other astronomers argued for a distinction between planets and dwarf planets based on the inability of the latter to `` clear the neighbourhood around their orbits '' : planets are able to remove smaller bodies near their orbits by collision, capture, or gravitational disturbance ( or establish orbital resonances that prevent collisions ), whereas dwarf planets lack the mass to do so. Soter went on to propose a parameter he called the planetary discriminant, designated with the symbol μ ( mu ), that represents an experimental measure of the actual degree of cleanliness of the orbital zone ( where μ is calculated by dividing the mass of the candidate body by the total mass of the other objects that share its orbital zone ), where μ > 100 is deemed to be cleared. Jean - Luc Margot refined Stern and Levison 's concept to produce a similar parameter Π ( Pi ). It is based on theory, avoiding the empirical data used by Λ. Π > 1 indicates a planet, and there is again a gap of several orders of magnitude between planets and dwarf planets. There are several other schemes that try to differentiate between planets and dwarf planets, but the 2006 definition uses this concept. Hydrostatic equilibrium Main article : Hydrostatic equilibrium Sufficient internal pressure, caused by the body 's gravitation, will turn a body plastic, and sufficient plasticity will allow high elevations to sink and hollows to fill in, a process known as gravitational relaxation. Bodies smaller than a few kilometers are dominated by non-gravitational forces and tend to have an irregular shape. Larger objects, where gravitation is significant but not dominant, are `` potato '' shaped ; the more massive the body is, the higher its internal pressure and the more rounded its shape, until the pressure is sufficient to overcome its internal compressive strength and it achieves hydrostatic equilibrium. At this point a body is as round as it is possible to be, given its rotation and tidal effects, and is an ellipsoid in shape. This is the defining limit of a dwarf planet. When an object is in hydrostatic equilibrium, a global layer of liquid covering its surface would form a liquid surface of the same shape as the body, apart from small - scale surface features such as craters and fissures. If the body does not rotate, it will be a sphere, but the faster it rotates, the more oblate or even scalene it becomes. If such a rotating body were to be heated until it melted, its overall shape would not change when liquid. The extreme example of a non-spherical body in hydrostatic equilibrium is Haumea, which is twice as long along its major axis as it is at the poles. If the body has a massive nearby companion, then tidal forces come into effect as well, distorting it into a prolate spheroid. An example of this is Jupiter 's moon Io, which is the most volcanically active body in the Solar System due to effects of tidal heating. Tidal forces also cause a body 's rotation to gradually become tidally locked, such that it always presents the same face to its companion. An extreme example of this is the Pluto -- Charon system, where both bodies are tidally locked to each other. Earth 's Moon is also tidally locked, as are many satellites of the gas giants. The masses of the IAU - recognized dwarf planets plus Charon relative to the Moon. The mass of Makemake is a rough estimate. ( See plutoid for a graph of several additional likely dwarf planets without Ceres. ) The upper and lower size and mass limits of dwarf planets have not been specified by the IAU. There is no defined upper limit, and an object larger or more massive than Mercury that has not `` cleared the neighbourhood around its orbit '' would be classified as a dwarf planet. The lower limit is determined by the requirements of achieving a hydrostatic equilibrium shape, but the size or mass at which an object attains this shape depends on its composition and thermal history. The original draft of the 2006 IAU resolution redefined hydrostatic equilibrium shape as applying `` to objects with mass above 5 × 10 kg and diameter greater than 800 km '', but this was not retained in the final draft. Empirical observations suggest that the lower limit will vary according to the composition and thermal history of the object. For a body made of rigid silicates, such as the stony asteroids, the transition to hydrostatic equilibrium should occur at a diameter of approximately 600 km and a mass of 3.4 × 10 kg. For a body made of less rigid water ice, the limit should be about 320 km and 10 kg. In the asteroid belt, Ceres is the only body that clearly surpasses the silicaceous limit ( though it is actually a rocky -- icy body ), and its shape is an equilibrium spheroid. 2 Pallas and 4 Vesta are rocky and are just below the limit. Pallas, at 525 -- 560 km and 1.85 -- 2.4 × 10 kg, is `` nearly round '' but still somewhat irregular. Vesta, at 530 km and 2.6 × 10 kg, deviates from an ellipsoid shape primarily due to a large impact basin at its pole. Dwarf planets and possible dwarf planets Illustration of the relative sizes, albedos, and colours of the largest trans - Neptunian objects Eight dwarves or Candidates and moon 's orbits, shown at angle Main article : List of possible dwarf planets Many trans - Neptunian objects ( TNOs ) are thought to have icy cores and therefore would require a diameter of perhaps 400 km ( 250 mi ) -- only about 3 % of that of Earth -- to relax into gravitational equilibrium. As of January 2015, about 150 known TNOs are considered potential dwarf planets, although only rough estimates of the diameters of most of these objects are available. A team is investigating thirty of these, and think that the number will eventually prove to be around 200 in the Kuiper belt, with thousands more beyond. Recognized The IAU has recognized five bodies as dwarf planets since 2008 : Ceres, Pluto, Eris, Haumea, and Makemake. Ceres and Pluto are known to be dwarf planets through direct observation. Eris is recognized as a dwarf planet because it is more massive than Pluto ( measurements by New Horizons indicate that Pluto 's diameter is larger than that of Eris ), whereas Haumea and Makemake qualify based on their absolute magnitudes. In relative distance from the Sun, the five are : Ceres -- discovered on January 1, 1801, 45 years before Neptune. Considered a planet for half a century before reclassification as an asteroid. Accepted as a dwarf planet by the IAU on September 13, 2006. Pluto ♇ -- discovered on February 18, 1930. Classified as a planet for 76 years. Reclassified as a dwarf planet by the IAU on August 24, 2006. Haumea -- discovered on December 28, 2004. Accepted by the IAU as a dwarf planet on September 17, 2008. Makemake -- discovered on March 31, 2005. Accepted by the IAU as a dwarf planet on July 11, 2008. Eris -- discovered on January 5, 2005. Called the `` tenth planet '' in media reports. Accepted by the IAU as a dwarf planet on September 13, 2006. Proposed Main article : List of possible dwarf planets Mike Brown considers an additional six trans - Neptunian objects to be `` nearly certainly '' dwarf planets with diameters at or above 900 kilometers. These objects are : Quaoar -- discovered on June 5, 2002 2002 MS -- discovered on June 18, 2002 Sedna -- discovered on November 14, 2003 Orcus -- discovered on February 17, 2004 Salacia -- discovered on September 22, 2004 2007 OR -- discovered on July 17, 2007 Tancredi et al. advised the IAU to officially accept Orcus, Sedna and Quaoar. In addition, Gonzalo Tancredi considers the five TNOs Varuna, Ixion, 2003 AZ, 2004 GV, and 2002 AW to be dwarf planets as well. Objects recognized by the IAU as dwarf planets Orbital attributes Name Region of the Solar System Orbital radius ( AU ) Orbital period ( years ) Mean orbital speed ( km / s ) Inclination to ecliptic Orbital eccentricity Planetary discriminant Ceres Asteroid belt 2.77 4.60 17.882 10.59 ° 0.079 0.33 Pluto Kuiper belt ( plutino ) 39.48 248.09 4.666 17.14 ° 0.249 0.077 Haumea Kuiper belt ( 12 : 7 ) 43.13 283.28 28.22 ° 0.195 0.020 Makemake Kuiper belt ( cubewano ) 45.79 309.9 4.419 28.96 ° 0.159 0.02 Eris Scattered disc 67.67 557 3.436 44.19 ° 0.442 0.10 Physical attributes Name Diameter relative to the Moon Diameter ( km ) Mass relative to the Moon Mass ( × 10 kg ) Density ( g / cm ) Surface gravity ( m / s ) Escape velocity ( km / s ) Axial inclination Rotation period ( days ) Moons Surface temp. ( K ) Atmosphere Ceres 27 % 946 1.3 % 0.94 2.17 0.29 0.51 ≈ 3 ° 0.38 0 167 none 3.3 Pluto 68 % 7003238000000000000 ♠ 2380 ± 0.4 17.8 % 13.05 1.87 0.58 119.59 ° − 6.39 5 44 transient − 0.76 Haumea ≈ 36 % 1632 7003124000000000000 ♠ 1240 + 69 − 58 5.5 % 7000401000000000000 ♠ 4.01 ± 0.04 1.885 -- 1.757 2.6 -- 3.3 ( ? ) 0.44 0.84 0.16 7001320000000000000 ♠ 32 ± 3 ? 0.2 Makemake 41 % 7003143000000000000 ♠ 1430 ± 14 ? ? > 1.4 ? 0.32 ≈ 30 none − 0.3 Eris 67 % 7003232600000000000 ♠ 2326 ± 12 22.7 % 16.7 2.5 ≈ 0.8 1.3 ≈ 1 ( 0.75 -- 1.4 ) ≈ 42 transient ? − 1.1 Additional objects recognized by Brown and Tancredi as dwarf planets Orbital attributes Name Region of the Solar System Orbital radius ( AU ) Orbital period ( years ) Mean orbital speed ( km / s ) Inclination to ecliptic Orbital eccentricity Planetary discriminant Orcus Kuiper belt ( plutino ) 39.17 245.18 20.57 ° 0.227 0.003 2002 MS Kuiper belt ( cubewano ) 41.931 271.53 17.693 ° 0.14135 Salacia Kuiper belt ( cubewano ) 42.1889 274.03 23.9396 ° 0.10312 Quaoar Kuiper belt ( cubewano ) 43.405 285.97 8.00 ° 0.039 0.007 -- 0.010 2007 OR Scattered disc ( 10 : 3 ) 67.21 550.98 30.70 ° 0.500 ? Sedna Detached 518.57 ≈ 11,400 11.93 ° 0.853 < 0.07 Physical attributes Name Diameter relative to the Moon Diameter ( km ) Mass relative to the Moon Mass ( × 10 kg ) Density ( g / cm ) Surface gravity ( m / s ) Escape velocity ( km / s ) Axial inclination Rotation period ( days ) Moons Surface temp. ( K ) Atmosphere Orcus 26 % 7002917000000000000 ♠ 917 ± 25 0.9 % 0.63 0.55 < 44 2002 MS ≈ 27 % 7002934000000000000 ♠ 934 ± 47 ? ? 0 ≈ 43 3.7 Salacia ≈ 25 % 7002854000000000000 ♠ 854 ± 45 0.6 % 0.45 7000115999999999999 ♠ 1.16 + 0.59 − 0.36 0.25 3.9 Quaoar 32 % 7003111000000000000 ♠ 1110 ± 5 1.8 -- 2.0 % 7000139999999999999 ♠ 1.4 ± 0.1 0.74 ≈ 43 2.4 2007 OR ≈ 44 % 7003153500000000000 ♠ 1535 + 75 − 225 ? 1.87 1.8 Sedna ≈ 30 % 7002995000000000000 ♠ 995 ± 80 ≈ 1.4 % ≈ 1 0.42 0 ≈ 12 1.5 Vesta, the next-most - massive body in the asteroid belt after Ceres, is roughly spherical, deviating mainly because of massive impacts that formed Rheasilvia and Veneneia crater after it solidified. Furthermore, its triaxial dimensions are not consistent with hydrostatic equilibrium. Triton is thought to be a captured dwarf planet. Phoebe is a captured body that, like Vesta, is no longer in hydrostatic equilibrium, but is thought to have been so early in its history. Exploration The dwarf planet Ceres, as imaged by NASA 's Dawn spacecraft. On March 6, 2015, the Dawn spacecraft began to orbit Ceres, becoming the first spacecraft to orbit a dwarf planet. On July 14, 2015, the New Horizons space probe flew by Pluto and its five moons. Dawn has also explored the former dwarf planet Vesta. Phoebe has been explored by Cassini ( most recently ) and Voyager 2, which also explored Triton. These three are thought to be former dwarf planets and therefore their exploration helps in the study of the evolution of dwarf planets. Contention In the immediate aftermath of the IAU definition of dwarf planet, some scientists expressed their disagreement with the IAU resolution. Campaigns included car bumper stickers and T - shirts. Mike Brown ( the discoverer of Eris ) agrees with the reduction of the number of planets to eight. NASA has announced that it will use the new guidelines established by the IAU. Alan Stern, the director of NASA 's mission to Pluto, rejects the current IAU definition of planet, both in terms of defining dwarf planets as something other than a type of planet, and in using orbital characteristics ( rather than intrinsic characteristics ) of objects to define them as dwarf planets. Thus, in 2011, he still referred to Pluto as a planet, and accepted other dwarf planets such as Ceres and Eris, as well as the larger moons, as additional planets. Several years before the IAU definition, he used orbital characteristics to separate `` überplanets '' ( the dominant eight ) from `` unterplanets '' ( the dwarf planets ), considering both types `` planets ''. Planetary - mass moons See also : List of natural satellites Nineteen moons are known to be massive enough to have relaxed into a rounded shape under their own gravity, and seven of them are more massive than either Eris or Pluto. They are not physically distinct from the dwarf planets, but are not dwarf planets because they do not directly orbit the Sun. The seven that are more massive than Eris are the Moon, the four Galilean moons of Jupiter ( Io, Europa, Ganymede, and Callisto ), one moon of Saturn ( Titan ), and one moon of Neptune ( Triton ). The others are six moons of Saturn ( Mimas, Enceladus, Tethys, Dione, Rhea, and Iapetus ), five moons of Uranus ( Miranda, Ariel, Umbriel, Titania, and Oberon ), and one moon of Pluto ( Charon ). There are additional possibilities among TNOs, including Dysnomia orbiting Eris. Alan Stern calls these moons `` satellite planets '', one of three categories of planet together with dwarf planets and classical planets. The term planemo ( `` planetary - mass object '' ) covers all three. In a draft resolution for the IAU definition of planet, both Pluto and Charon would have been considered dwarf planets in a binary system, given that they both satisfied the mass and shape requirements for dwarf planets and revolved around a common center of mass located between the two bodies ( rather than within one of the bodies ). The IAU currently states that Charon is not considered to be a dwarf planet and is just a satellite of Pluto, although the idea that Charon might qualify to be a dwarf planet in its own right may be considered at a later date. The location of the barycenter depends not only on the relative masses of the bodies, but also on the distance between them ; the barycenter of the Sun -- Jupiter orbit, for example, lies outside the Sun. See also Book : Dwarf Planets of the Solar System & Their Satellites Book : Solar System Centaur List of gravitationally rounded objects of the Solar System List of planetary bodies List of possible dwarf planets List of Solar System bodies formerly regarded as planets Lists of small Solar System bodies Mesoplanet Notes Jump up ^ The footnote in the original text reads : For two or more objects comprising a multiple object system... A secondary object satisfying these conditions i.e. that of mass, shape is also designated a planet if the system barycentre resides outside the primary. Secondary objects not satisfying these criteria are `` satellites ''. Under this definition, Pluto 's companion Charon is a planet, making Pluto -- Charon a double planet. References ^ Jump up to : IAU ( August 24, 2006 ). `` Definition of a Planet in the Solar System : Resolutions 5 and 6 '' ( PDF ). IAU 2006 General Assembly. International Astronomical Union. Retrieved January 26, 2008. Jump up ^ Brown, Michael E. ; Schaller, Emily L. ( June 15, 2007 ). `` The Mass of Dwarf Planet Eris ''. Science. 316 ( 5831 ) : 1585. Bibcode : 2007Sci... 316.1585 B. doi : 10.1126 / science. 1139415. PMID 17569855. Jump up ^ Koski, Olivia ( December 27, 2010 ). `` Q&A : Astronomer Mike Brown on How He Killed Pluto ''. Wired. Retrieved February 12, 2012. Jump up ^ Perlman, David ( August 25, 2006 ). `` Pluto demoted -- from 9th planet to just a dwarf ''. San Francisco Chronicle. Retrieved February 12, 2012. Jump up ^ Kennedy, Stephanie ( August 25, 2006 ). `` Pluto stripped of planet status ''. `` AM '', ABC Local Radio. Retrieved February 12, 2012. ^ Jump up to : Rincon, Paul ( August 25, 2006 ). `` Pluto vote ' hijacked ' in revolt ''. BBC News. Retrieved January 26, 2008. Jump up ^ Jorge Salazar ( November 30, 2009 ). `` Alan Stern : ' A Chihuahua is still a dog, and Pluto is still a planet ' ''. EarthSky ( Earthsky Interviews ). Retrieved December 8, 2009. Jump up ^ S. Alan Stern, `` On the number of planets in the outer solar system : Evidence of a substantial population of 1000 - km bodies '', Icarus 90 : 2, April 1991 ^ Jump up to : `` Dwarf Planets and their Systems ''. Working Group for Planetary System Nomenclature ( WGPSN ). July 11, 2008. Retrieved July 13, 2008. ^ Jump up to : `` Free the Dwarf Planets ! ''. Michael Brown. August 24, 2011. Retrieved August 24, 2011. ^ Jump up to : Mike Brown, ' How many dwarf planets are there in the outer solar system ? ' Archived October 18, 2011, at the Wayback Machine. Accessed November 15, 2013 ^ Jump up to : Stern, Alan ( August 24, 2012 ). The PI 's Perspective. Archived November 13, 2014, at the Wayback Machine., August 24, 2012. Retrieved from http://pluto.jhuapl.edu/overview/piPerspective.php?page=piPerspective_08_24_2012. Jump up ^ Mike Brown, ' How many dwarf planets are there in the outer solar system ? ' Archived October 18, 2011, at the Wayback Machine. Accessed February 5, 2018 Jump up ^ Dan Bruton. `` Conversion of Absolute Magnitude to Diameter for Minor Planets ''. Department of Physics & Astronomy ( Stephen F. Austin State University ). Archived from the original on March 23, 2010. Retrieved June 13, 2008. ^ Jump up to : `` Plutoid chosen as name for Solar System objects like Pluto '' ( Press release ). ^ Jump up to : `` The IAU draft definition of `` planet '' and `` plutons '' ``. International Astronomical Union. August 16, 2006. Retrieved May 17, 2008. Jump up ^ Mauro Murzi ( 2007 ). `` Changes in a scientific concept : what is a planet ? ''. Retrieved April 6, 2013. ( Preprint ) Jump up ^ Mager, Brad. `` Pluto Revealed ''. discoveryofpluto.com. Retrieved January 26, 2008. Jump up ^ Cuk, Matija ; Masters, Karen ( September 14, 2007 ). `` Is Pluto a planet ? ''. Cornell University, Astronomy Department. Archived from the original on October 12, 2007. Retrieved January 26, 2008. Jump up ^ Buie, Marc W. ; Grundy, William M. ; Young, Eliot F. ; Young, Leslie A. ; Stern, S. Alan ( 2006 ). `` Orbits and Photometry of Pluto 's Satellites : Charon, S / 2005 P1, and S / 2005 P2 ''. The Astronomical Journal. 132 ( 1 ) : 290 -- 98. arXiv : astro - ph / 0512491. Bibcode : 2006AJ... 132... 290B. doi : 10.1086 / 504422. Retrieved February 10, 2008. Jump up ^ Jewitt, David ; Delsanti, Audrey ( 2006 ). The Solar System Beyond The Planets in Solar System Update : Topical and Timely Reviews in Solar System Sciences ( PDF ) ( PDF ). Springer. doi : 10.1007 / 3 - 540 - 37683 - 6. ISBN 978 - 3 - 540 - 37683 - 5. Archived from the original ( PDF ) on May 25, 2006. Retrieved February 10, 2008. Jump up ^ Weintraub, David A. ( 2006 ). Is Pluto a Planet ? A Historical Journey through the Solar System. Princeton, N.J. : Princeton Univ. Press. pp. 1 -- 272. ISBN 978 - 0 - 691 - 12348 - 6. Jump up ^ Phillips, Tony ; Phillips, Amelia ( September 4, 2006 ). `` Much Ado about Pluto ''. PlutoPetition.com. Archived from the original on January 25, 2008. Retrieved January 26, 2008. Jump up ^ `` Planetoids Beyond Pluto ''. Astrobiology Magazine. December 30, 2004. Retrieved January 26, 2008. Jump up ^ `` Hubble Observes Planetoid Sedna, Mystery Deepens ''. NASA 's Hubble Space Telescope home site. April 14, 2004. Retrieved January 26, 2008. Jump up ^ Brown, Michael E. `` The Discovery of Eris, the Largest Known Dwarf Planet ''. California Institute of Technology, Department of Geological Sciences. Retrieved January 26, 2008. Jump up ^ Brown, Michael E. ( 2004 ). `` What is the definition of a planet ? ''. California Institute of Technology, Department of Geological Sciences. Retrieved January 26, 2008. Jump up ^ Brown, Mike ( August 16, 2006 ). `` War of the Worlds ''. New York Times. Retrieved February 20, 2008. Jump up ^ California Institute of Technology, Retrieved 4 - 12 - 2015 Jump up ^ `` Astronomers Measure Mass of Largest Dwarf Planet ''. NASA 's Hubble Space Telescope home site. June 14, 2007. Retrieved January 26, 2008. Jump up ^ Brown, Michael E. `` What makes a planet ? ''. California Institute of Technology, Department of Geological Sciences. Retrieved January 26, 2008. ^ Jump up to : Britt, Robert Roy ( August 19, 2006 ). `` Details Emerge on Plan to Demote Pluto ''. Space.com. Retrieved August 18, 2006. Jump up ^ Karttunen ; et al., eds. ( 2007 ). Fundamental Astronomy ( 5 ed. ). Springer. ^ Jump up to : Brown, Mike ( 2010 ). How I Killed Pluto and Why It Had It Coming. Spiegel & Grau. p. 223. Jump up ^ Bailey, Mark E. `` Comments & discussions on Resolution 5 : The definition of a planet -- Planets Galore ''. Dissertatio cum Nuncio Sidereo, Series Tertia -- official newspaper of the IAU General Assembly 2006. Astronomical Institute Prague. Retrieved February 9, 2008. Jump up ^ `` Dos uruguayos, Julio Fernández y Gonzalo Tancredi en la historia de la astronomía : reducen la cantidad de planetas de 9 a 8... &Anotaciones de Tancredi '' ( in Spanish ). Science and Research Institute, Mercedes, Uruguay. Archived from the original on December 20, 2007. Retrieved February 11, 2008. Jump up ^ IAU ( 2009 ). Reports on Astronomy 2006 -- 2009. Transactions of the IAU, vol. XXVII - A ^ Jump up to : `` IAU 2006 General Assembly : Result of the IAU Resolution votes ''. Jump up ^ IAU ( 2009 ). Division III ( Planetary Systems Sciences ) : Triennial Report 2006 -- 2009. Transactions IAU, Volume XXVIIA ^ Jump up to : Soter, Steven ( August 16, 2006 ). `` What is a Planet ? ''. The Astronomical Journal. 132 ( 6 ) : 2513 -- 19. arXiv : astro - ph / 0608359. Bibcode : 2006AJ... 132.2513 S. doi : 10.1086 / 508861. Jump up ^ Calculated using the estimate of a minimum of 15 Sedna mass objects in the region. Estimate found in Schwamb, Megan E ; Brown, Michael E ; Rabinowitz, David L ( 2009 ). `` A Search for Distant Solar System Bodies in the Region of Sedna ''. The Astrophysical Journal. 694 ( 1 ) : L45 -- 8. arXiv : 0901.4173. Bibcode : 2009ApJ... 694L... 45S. doi : 10.1088 / 0004 - 637X / 694 / 1 / L45. ^ Jump up to : Stern, S. Alan ; Levison, Harold F. ( 2002 ). `` Regarding the criteria for planethood and proposed planetary classification schemes '' ( PDF ). Highlights of Astronomy. 12 : 205 -- 213, as presented at the XXIVth General Assembly of the IAU -- 2000 ( Manchester, UK, August 7 -- 18, 2000 ). Bibcode : 2002HiA... 12... 205S. ^ Jump up to : Margot, Jean - Luc ( October 15, 2015 ). `` A Quantitative Criterion for Defining Planets ''. The Astronomical Journal. 150 ( 6 ) : 185. arXiv : 1507.06300. Bibcode : 2015AJ... 150... 185M. doi : 10.1088 / 0004 - 6256 / 150 / 6 / 185. Jump up ^ Lineweaver & Marc Norman, 2010, `` The Potato Radius : a Lower Minimum Size for Dwarf Planets '' Jump up ^ Indeed, Mike Brown has set out to find such an object. ( `` Julia Sweeney and Michael E. Brown ''. Hammer Conversations : KCET podcast. 2007. Archived from the original on June 26, 2008. Retrieved June 28, 2008. ) Jump up ^ G.H.A. Cole, 2000, Minimum Radius And Mass For A Planetary Body, archived from the original on June 6, 2011 ^ Jump up to : Brown, Michael E. `` The Dwarf Planets ''. California Institute of Technology, Department of Geological Sciences. Retrieved January 26, 2008. Jump up ^ `` IAU names fifth dwarf planet Haumea ''. Paris : International Astronomical Union. September 17, 2008. Retrieved September 16, 2011. ^ Jump up to : Tancredi, G. ; Favre, S.A. ( 2008 ). `` Which are the dwarfs in the Solar System ? ''. Icarus. 195 ( 2 ) : 851 -- 862. Bibcode : 2008Icar... 195... 851T. doi : 10.1016 / j. icarus. 2007.12. 020. ^ Jump up to : Bowell, Ted. `` The Asteroid Orbital Elements Database ''. Lowell Observatory. Retrieved February 12, 2008. ^ Jump up to : Ortiz, J.L. ; Santos - Sanz, P. ; Sicardy, B. ; et al. ( 2017 ). `` The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation ''. Nature. 550 ( 7675 ) : 219 -- 223. Bibcode : 2017Natur. 550... 219O. doi : 10.1038 / nature24051. Jump up ^ Fornasier, S. ; Lellouch, E. ; Müller, T. ; Santos - Sanz, P. ; Panuzzo, P. ; Kiss, C. ; Lim, T. ; Mommert, M. ; Bockelée - Morvan, D. ; Vilenius, E. ; Stansberry, J. ; Tozzi, G.P. ; Mottola, S. ; Delsanti, A. ; Crovisier, J. ; Duffard, R. ; Henry, F. ; Lacerda, P. ; Barucci, A. ; Gicquel, A. ( 2013 ). `` '' TNOs are cool `` : A survey of the trans - Neptunian region VIII. Combined Herschel PACS and SPIRE observations of nine bright targets at 70 -- 500 μm '' ( PDF ). Astronomy and Astrophysics. 555 : A15. arXiv : 1305.0449. Bibcode : 2013A&A... 555A... 15F. doi : 10.1051 / 0004 - 6361 / 201321329. Jump up ^ M.E. Brown, 2013, `` On the size, shape, and density of dwarf planet Makemake '' Jump up ^ European Southern Observatory. `` Dwarf Planet Makemake Lacks Atmosphere : Distant Frigid World Reveals Its Secrets for First Time ''. ScienceDaily. Retrieved November 19, 2012. Jump up ^ Thomas, Peter C. ; Binzelb, Richard P. ; Gaffeyc, Michael J. ; Zellnerd, Benjamin H. ; Storrse, Alex D. ; Wells, Eddie ( 1997 ). `` Vesta : Spin Pole, Size, and Shape from HST Images ''. Icarus. 128 ( 1 ) : 88 -- 94. Bibcode : 1997Icar... 128... 88T. doi : 10.1006 / icar. 1997.5736. Jump up ^ Asmar, S.W. ; Konopliv, A.S. ; Park, R.S. ; Bills, B.G. ; Gaskell, R. ; Raymond, C.A. ; Russell, C.T. ; Smith, D.E. ; Toplis, M.J. ; Zuber, M.T. ( 2012 ). `` The Gravity Field of Vesta and Implications for Interior Structure '' ( PDF ). 43rd Lunar and Planetary Science Conference : 2600. Bibcode : 2012LPI... 43.2600 A. Jump up ^ Russel, C.T. ; et al. ( 2012 ). `` Dawn at Vesta : Testing the Protoplanetary Paradigm '' ( PDF ). Science. 336 ( 6082 ) : 684 -- 686. Bibcode : 2012Sci... 336... 684R. doi : 10.1126 / science. 1219381. PMID 22582253. Jump up ^ Agnor, C.B. ; Hamilton, D.P. ( 2006 ). `` Neptune 's capture of its moon Triton in a binary -- planet gravitational encounter '' ( PDF ). Nature. 441 ( 7090 ) : 192 -- 4. Bibcode : 2006Natur. 441... 192A. doi : 10.1038 / nature04792. PMID 16688170. Jump up ^ JPL / NASA, 2012 Apr 26. Cassini Finds Saturn Moon Has Planet - Like Qualities Jump up ^ Landau, Elizabeth ; Brown, Dwayne ( March 6, 2015 ). `` NASA Spacecraft Becomes First to Orbit a Dwarf Planet ''. NASA. Retrieved March 6, 2015. Jump up ^ Chang, Alicia ( August 25, 2006 ). `` Online merchants see green in Pluto news ''. Associated Press. USA Today. Retrieved January 25, 2008. Jump up ^ Brown, Michael E. `` The Eight Planets ''. California Institute of Technology, Department of Geological Sciences. Retrieved January 26, 2008. Jump up ^ `` Hotly - Debated Solar System Object Gets a Name ''. NASA press release. September 14, 2006. Retrieved January 26, 2008. Jump up ^ Stern, Alan ( September 6, 2006 ). `` Unabashedly Onward to the Ninth Planet ''. New Horizons Web Site. Archived from the original on December 7, 2013. Retrieved January 26, 2008. Jump up ^ Wall, Mike ( August 24, 2011 ). `` Pluto 's Planet Title Defender : Q & A With Planetary Scientist Alan Stern ''. SPACE.com. Retrieved December 3, 2012. ^ Jump up to : `` Should Large Moons Be Called ' Satellite Planets ' ? ''. News.discovery.com. May 14, 2010. Retrieved November 4, 2011. Jump up ^ Basri, G. ; Brown, M.E. ( 2006 ). `` Planetesimals to Brown Dwarfs : What is a Planet ? '' ( PDF ). Annual Review of Earth and Planetary Sciences. 34 : 193 -- 216. arXiv : astro - ph / 0608417. Bibcode : 2006AREPS... 34... 193B. doi : 10.1146 / annurev. earth. 34.031405. 125058. Archived from the original ( PDF ) on July 31, 2013. Jump up ^ `` Pluto and the Solar System ''. IAU. Retrieved July 10, 2013. External links Look up dwarf planet in Wiktionary, the free dictionary. Wikimedia Commons has media related to Dwarf planets. NPR : Dwarf Planets May Finally Get Respect ( David Kestenbaum ) BBC News : Q&A New planets proposal, August 16, 2006 Ottawa Citizen : The case against Pluto ( P. Surdas Mohit ) August 24, 2006 James L. Hilton, When Did the asteroids Become Minor Planets ? NASA : IYA 2009 Dwarf Planets Dwarf planets Asteroid belt IAU : Ceres No longer rounded and therefore no longer dwarf planets ( Vesta ) Centaurs Possibly : Chariklo Chiron Centaurs ( extended ) Possibly : 1995 SN 55 ( lost ) Ceto 2010 TY 53 Plutinos IAU : Pluto Additional objects proposed by Brown and Tancredi : Orcus Ixion 2003 AZ 2004 UX Huya Possibly : 2003 UZ 2003 VS 2002 VR 2004 PF 2002 XV 93 2007 JH 43 2001 QF 298 Twotinos Possibly : 2002 WC Other resonances / unknown resonances : IAU : Haumea Possibly : 2002 XW 1999 DE 1999 KR 2001 YH 2011 GM 27 2010 VK 201 2013 FZ 27 2014 UM 33 1999 CD 158 Cubewanos : IAU : Makemake Additional objects proposed by Brown and Tancredi : 2002 MS Salacia Quaoar Varuna Varda 2004 GV 2002 AW 2002 TX 2005 RR 2003 OP 2005 RN Possibly : Chaos Altjira Sila - Nunam 2002 UX 2007 JJ 2005 UQ 2004 TY 2003 QW 1998 SN 2002 KX Praamzius 2004 NT 2010 FX 86 2002 CY 248 2010 VR 11 Rhadamanthus Scattered disc IAU : Eris Additional objects proposed by Brown and Tancredi : 2007 OR 1996 TL 2001 UR 2005 RM Possibly : 2002 TC 2004 XA 2005 QU 2006 QH 181 2007 UK 2010 EK 139 2010 KZ 39 2010 RE 64 2010 RF 43 2010 TJ 2013 FY 27 2008 OG 19 1996 GQ 2012 HH 1999 CC 2010 VZ 98 Area uncertain Captured satellites that were once dwarf planets : Triton ( captured by Neptune ) Phoebe ( captured by Saturn, and no longer rounded ) Possibly : 2011 FW 62 ( lost ) 2000 YW V774104 Detached objects Possibly : 2004 XR 190 2010 GB 174 2008 ST 291 1995 TL 2005 TB 2003 QX 113 2003 FY 2004 VN 112 2000 CR Sednoids Objects proposed by Brown and Tancredi : Sedna Possibly : 2012 VP 113 See also : Charon Vanth Dysnomia Hiʻiaka Mesoplanet Planemo List of trans - Neptunian objects List of possible dwarf planets List of Solar System objects List of Solar System objects by size The Solar System The Sun Mercury Venus Earth Mars Ceres Jupiter Saturn Uranus Neptune Pluto Haumea Makemake Eris Planets and Dwarf planets Terrestrial planets Mercury Venus Earth Mars Giant planets Jupiter Saturn Uranus Neptune Dwarf planets Ceres Pluto Haumea Makemake Eris Rings Jovian Saturnian ( Rhean ) Charikloan Chironean Uranian Neptunian Haumean Moons Terrestrial Moon other near - Earth objects Martian Phobos Deimos Jovian Ganymede Callisto Io Europa all 79 Saturnian Titan Rhea Iapetus Dione Tethys Enceladus Mimas Hyperion Phoebe all 62 Uranian Titania Oberon Umbriel Ariel Miranda all 27 Neptunian Triton Proteus Nereid all 14 Plutonian Charon Nix Hydra Kerberos Styx Haumean Hiʻiaka Namaka Makemakean S / 2015 ( 136472 ) 1 Eridian Dysnomia Lists Solar System objects By size By discovery date Minor planets Gravitationally rounded objects Possible dwarf planets Natural satellites Comets Small Solar System bodies Meteoroids Minor planets moons Comets Damocloids Mercury - crossers Venus - crossers Venus trojans Near - Earth objects Earth - crossers Earth trojans Mars - crossers Mars trojans Asteroid belt Asteroids first discovered : Ceres Pallas Juno Vesta Families Notable asteroids Kirkwood gap Main - belt comets Jupiter trojans Jupiter - crossers Centaurs Saturn - crossers Uranus trojans Uranus - crossers Neptune trojans Cis - Neptunian objects Trans - Neptunian objects Neptune - crossers Plutoids Kuiper belt Plutinos Cubewanos Scattered disc Detached objects Sednoids Hills cloud Oort cloud Hypothetical objects Vulcan Vulcanoids Phaeton Planet V Theia Fifth giant Planets beyond Neptune Tyche Nemesis Planet Nine Exploration ( outline ) Discovery Astronomy Timeline Spaceflight Robotic spacecraft Human spaceflight List of crewed spacecraft Colonization List of probes Timeline Mercury Venus Moon Mars Ceres Asteroids Mining Comets Jupiter Saturn Uranus Neptune Pluto Deep space Outline of the Solar System Portals Solar System Astronomy Earth sciences Mars Jupiter Uranus Cosmology Solar System → Local Interstellar Cloud → Local Bubble → Gould Belt → Orion Arm → Milky Way → Milky Way subgroup → Local Group → Local Sheet → Virgo Supercluster → Laniakea Supercluster → Observable universe → Universe Each arrow ( → ) may be read as `` within '' or `` part of ''. 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Question: what is the name of the dwarf planets
Answer: Ceres