225088 Gonggong

225088 Gonggong (provisional designation: 2007 OR10) is a likely dwarf planet of the Solar System, and a member of the scattered disc beyond Neptune. It has a highly eccentric and inclined orbit during which it ranges from 34–101 astronomical units (5.1–15.1 billion kilometers; 3.2–9.4 billion miles) from the Sun. As of 2019, its distance from the Sun is 88 AU (13.2×10^9 km; 8.2×10^9 mi), and it is the sixth-farthest known Solar System object. Gonggong is in a 3:10 orbital resonance with Neptune, in which it completes three orbits around the Sun for every ten orbits completed by Neptune. Gonggong was discovered in July 2007 by American astronomers Megan Schwamb, Michael Brown, and David Rabinowitz at the Palomar Observatory, and the discovery was announced in January 2009.

225088 Gonggong
Gonggong and its moon Xiangliu (red circle) seen by the Hubble Space Telescope in 2010
Discovery [1][2]
Discovered byMegan Schwamb
Michael E. Brown
David L. Rabinowitz
Discovery sitePalomar Obs.
Discovery date17 July 2007 [lower-alpha 1]
Designations
(225088) Gonggong
Pronunciation/ˈɡɒŋɡɒŋ/
Named after
共工 Gònggōng
2007 OR10
TNO [3] · SDO [4]
3:10 res.[5][6] · p-DP [7]
Orbital characteristics [3]
Epoch 31 May 2020 (JD 2459000.5)
Uncertainty parameter 4
Observation arc30.09 yr (10,989 days)
Earliest precovery date19 August 1985
Aphelion101.238 AU (15.145 Tm)
Perihelion33.703 AU (5.042 Tm)
67.471 AU (10.093 Tm)
Eccentricity0.50048
554.22 yr (202,003 days)
106.020°
0° 0m 6.402s / day
Inclination30.6569°
336.854°
207.666°
Known satellites1 (Xiangliu)
Physical characteristics
Mean diameter
1230±50 km[8]
Flattening0.03 (for a rotation period of 22.4 h)[8]
0.007 (for a rotation period of 44.81 h)[8]
Mass(1.75±0.07)×1021 kg[8]
Mean density
1.74±0.16 g/cm3[8]
Equatorial surface gravity
≈ 0.31 m/s2
Equatorial escape velocity
≈ 0.62 km/s
22.40±0.18 h or 44.81±0.37 h
(ambiguous,[9][10] but 22.4 h more likely[8])
0.14±0.01[8]
B−V=1.38±0.03[11][12]
V−R=0.86±0.02[11][12]
V−I=1.65±0.028[11][12]
21.4[13]
2.34[9] · 2.0[7]
1.8[3] · 1.6 (assumed)[1]

    At about 1,230 km (760 mi) in diameter, Gonggong is approximately the size of Pluto's moon Charon, and is the fifth-largest known trans-Neptunian object in the Solar System (not counting Charon). It may be sufficiently massive to be gravitationally rounded and therefore a dwarf planet. Gonggong's large mass makes retention of a tenuous atmosphere of methane just possible, though such an atmosphere would slowly escape into space. The object is named after Gònggōng, a Chinese water god responsible for chaos, floods and the tilt of the Earth. The name was chosen by its discoverers in 2019, when they hosted an online poll for the general public to help choose a name for the object, and the name Gonggong won.

    Gonggong is red, likely due to the presence of organic compounds called tholins on its surface. Water ice is also present on its surface, which hints at a brief period of cryovolcanic activity in the distant past. With a rotation period around 22 hours, Gonggong rotates slowly compared to other trans-Neptunian objects, which typically have periods less than 12 hours. The slow rotation of Gonggong may have been caused by tidal forces from its natural satellite, named Xiangliu.

    History

    Discovery
    Gonggong was discovered using the Samuel Oschin telescope at Palomar Observatory

    Gonggong was discovered by American astronomers Megan Schwamb, Michael Brown and David Rabinowitz on 17 July 2007.[1] The discovery was part of the Palomar Distant Solar System Survey, a survey conducted to find distant objects in the region of Sedna, beyond 50 AU (7.5×109 km; 4.6×109 mi) from the Sun, using the Samuel Oschin telescope at Palomar Observatory near San Diego, California.[14][15][16] The survey was designed to detect the movements of objects out to at least 1,000 AU from the Sun.[16] Schwamb identified Gonggong by comparing images using the blinking technique.[15] In the discovery images, Gonggong appeared to move slowly, suggesting that it is a distant object.[15][17] The discovery was part of Schwamb's doctoral thesis. At that time, Schwamb was a graduate student of Michael Brown at the California Institute of Technology.[18][15]

    Gonggong was formally announced in a Minor Planet Electronic Circular on 7 January 2009.[2] It was then given the provisional designation 2007 OR10 because it was discovered during the second half of July 2007.[2] The last letter and numbers of its designation indicate that it is the 267th object discovered during the latter half of July.[lower-alpha 2] As of April 2017, it has been observed 230 times over 13 oppositions, and has been identified in two precovery images, with the earliest image taken by the La Silla Observatory on 19 August 1985.[1][20]

    Naming

    The object is named after Gonggong, a water god in Chinese mythology. Gonggong is depicted as having a copper-and-iron, red-haired human head (or sometimes torso) and the body or tail of a serpent. Gonggong was responsible for creating chaos and catastrophe, causing flooding and tilting the Earth, until he was sent into exile.[21] Gonggong is often accompanied by his minister, Xiangliu, a nine-headed poisonous snake monster who was also responsible for causing flooding and destruction.[1]

    Before its official naming, Gonggong was the largest known unnamed object in the Solar System.[22] Initially after the discovery of Gonggong, Brown nicknamed the object "Snow White" for its presumed white color based on his assumption that it may be a member of the icy Haumea collisional family.[23][24] The nickname also fitted because, by that time, Brown's team had discovered seven other large trans-Neptunian objects which were collectively referred to as the "seven dwarfs":[25] Quaoar in 2002, Sedna in 2003, Haumea, Salacia and Orcus in 2004, and Makemake and Eris in 2005. However, Gonggong turned out to be very red in color, comparable to Quaoar, so the nickname was dropped.[23][17] On 2 November 2009, two years after its discovery, the Minor Planet Center assigned the minor planet number 225088 to Gonggong.[20]

    Upon the discovery and announcement of Gonggong, Brown did not consider naming it, as he regarded it to be an unremarkable object, despite its large size.[24][26] Brown later declared in 2011 that he now had enough information to justify giving it a name, in consideration of the discovery of water ice and the possibility of methane on its surface, which made it noteworthy enough to warrant further study.[18] Following the Kepler spacecraft's large revision of Gonggong's size in 2016, Schwamb justified that Gonggong was eligible for naming, an acknowledgement of its large size and that the characteristics of Gonggong were known with enough certainty for a name to be given to reflect them.[22]

    In 2019, the discoverers of Gonggong hosted an online poll for the general public to choose between three possible names: Gonggong (Chinese), Holle (German), and Vili (Norse). These were selected by the discoverers in accordance with the International Astronomical Union's (IAU's) minor planet naming criteria, which state that objects with orbits like that of Gonggong must be given names related to mythological figures that are associated with creation.[27][28] The three options were chosen because they were associated with water, ice, snow, and the color red—all characteristics of Gonggong—and because they had associated figures that could later provide a name for Gonggong's satellite.[29] The name for Gonggong's satellite was not chosen by the hosts of the naming poll, as this privilege is reserved for its discoverers.[27][21]

    Having gained 46 percent of the 280,000 votes, on 29 May 2019, the discovery team announced Gonggong as the winning name.[21] The name was proposed to the IAU's Committee on Small Body Nomenclature (CSBN), which is responsible for naming minor planets.[21] The name was accepted by the CSBN and was announced by the Minor Planet Center on 5 February 2020.[30]

    Physical characteristics

    Surface and spectra
    Artist's impression of Gonggong depicting its red surface

    The surface of Gonggong has an albedo (reflectivity) of 0.14.[8] The surface composition and spectrum of Gonggong is expected to be similar to that of Quaoar, as both objects are red in color and display signs of water ice and possibly methane in their spectra.[31][32] The reflectance spectrum of Gonggong was first measured in 2011 at near-infrared wavelengths, with the Folded port InfraRed Echellette (FIRE) spectrograph on the Magellan Baade Telescope at the Las Campanas Observatory in Chile.[33] Gonggong's spectrum exhibits a strong red spectral slope along with broad absorption bands at wavelengths of 1.5 μm and 2 μm, meaning that Gonggong reflects more light at these wavelengths.[33] Additional photometric measurements from the Hubble Space Telescope's Wide Field Camera 3 instrument display similar absorption bands at 1.5 μm,[33] which are characteristic features of water ice, a substance often found on large Kuiper belt objects.[34] The presence of water ice on the surface of Gonggong implies a brief period of cryovolcanism in the distant past, when water erupted from its interior, deposited onto its surface, and subsequently froze.[35]

    Gonggong is among the reddest trans-Neptunian objects known, especially in the visible and near-infrared.[33][11] Its red color is unexpected for an object with a substantial amount of water ice on its surface,[35][18] which are typically neutral in color, hence why Gonggong was initially nicknamed "Snow White".[23][24] Gonggong's color implies that methane is present on its surface, although it was not directly detected in the spectrum of Gonggong due to the low signal-to-noise ratio of the data.[33] The presence of methane frost would account for its color, as a result of the photolysis of methane by solar radiation and cosmic rays producing reddish organic compounds known as tholins.[33][9] Observations of Gonggong's near-infrared spectrum in 2015 revealed an absorption feature at 2.27 μm, indicating the presence of methanol along with its irradiation products on its surface.[36] Methanol is expected to brighten Gonggong's surface, although the irradiation of water ice may account for its present dark surface.[36]

    Gonggong is large enough to be able to retain trace amounts of volatile methane on its surface,[33] even when at its closest distance to the Sun (33.7 AU),[3] where temperatures are higher than that of Quaoar.[33] In particular, the large size of Gonggong means that it is likely to retain trace amounts of other volatiles, including ammonia, carbon monoxide, and possibly nitrogen, which almost all trans-Neptunian objects lose over the course of their existence.[31][9][22] Like Quaoar, Gonggong is expected to be near the mass limit at which it is able to retain those volatile materials on its surface.[31][18]

    Atmosphere
    Gonggong compared to the Earth and the Moon

    The presence of tholins on the surface of Gonggong implies the possible existence of a tenuous methane atmosphere, analogous to Quaoar.[35][18] Although Gonggong occasionally comes closer to the Sun than Quaoar, where it becomes warm enough that a methane atmosphere should evaporate, its larger mass could make the retention of methane just possible.[33] During aphelion, methane along with other volatiles would condense on Gonggong's surface, allowing for long-term irradiation that would otherwise result in a decrease in surface albedo.[37] The lower surface albedo would contribute to the loss of highly volatile materials such as nitrogen, as a lower albedo corresponds to more light being absorbed by the surface rather than being reflected, thus resulting in greater surface heating. Hence, the nitrogen content of Gonggong's atmosphere is expected to be depleted to trace amounts while methane is likely retained.[37]

    Gonggong is thought to have had cryovolcanic activity along with a more substantial atmosphere shortly after its formation.[35][18] Such cryovolcanic activity is expected to have been brief, and the resulting atmosphere gradually escaped over time.[35][18] Volatile gases, such as nitrogen and carbon monoxide, were lost, while less volatile gases such as methane are likely to remain in its present tenuous atmosphere.[35][37]

    Size
    Size estimates
    YearDiameterMethodRefs
    2010 1,752 km thermal [38]
    2011 1,200+300
    −200     km    		 best fit albedo [33]
    2012 1,280±210 km thermal [32]
    2013 1,142+647
    −467     km    		 thermal [39]
    2013 1,290 km radiometric [7]
    2016 1,535+75
    −225     km    		 thermal [9]
    2018 1,230±50 km radiometric [8]
    Comparison of sizes, albedo, and colors of various large trans-Neptunian objects. The gray arcs represent uncertainties of the object's size.
    Artistic comparison of Pluto, Eris, Haumea, Makemake, Gonggong, Quaoar, Sedna, Orcus, Salacia, 2002 MS4, and Earth along with the Moon.

    As of 2019, Gonggong is estimated to have a diameter of 1,230 km (760 mi), derived from radiometric measurements, its calculated mass, and assuming a density similar to other similar bodies.[8] This would make Gonggong the fifth-largest trans-Neptunian object, after Pluto, Eris, Haumea and Makemake. Gonggong is approximately the size of Pluto's moon Charon, although Gonggong's current size estimate has an uncertainty of 50 km (31 mi).[8]

    The International Astronomical Union (IAU) has not addressed the possibility of officially accepting additional dwarf planets since the acceptance of Makemake and Haumea in 2008, prior to the announcement of Gonggong in 2009.[40][41] Despite not satisfying the IAU's criterion of having an absolute magnitude brighter than +1,[40][lower-alpha 3] Gonggong is large enough to be considered a dwarf planet by several astronomers.[38][42][7] Brown states that Gonggong "must be a dwarf planet even if predominantly rocky", based on the 2013 radiometric measurement of 1,290 km (800 mi).[7] Scott Sheppard and colleagues think that it is likely to be a dwarf planet,[42] based on its minimum possible diameter—580 km (360 mi) under the assumption of a completely reflective surface with an albedo of 1[lower-alpha 4]—and what was at the time the expected lower size limit of around 200 km (120 mi) for hydrostatic equilibrium in cold icy-rocky bodies.[42] However, Iapetus is not in equilibrium despite being 1,470 km (910 mi) in diameter, so this remains just a possibility.[44]

    In 2010, astronomer Gonzalo Tancredi initially estimated Gonggong to have a very large diameter of 1,752 km (1,089 mi), though its dwarf planet status was unclear as there was no lightcurve data or other information to ascertain its size.[38] Gonggong is too distant to be resolved directly; Brown placed a rough estimate of its diameter ranging from 1,000–1,500 km (620–930 mi), based on an albedo of 0.18 which was the best fit in his model.[33] A survey led by a team of astronomers using the European Space Agency's Herschel Space Observatory in 2012 determined its diameter to be 1280±210 km (795±130 mi), based on the thermal properties of Gonggong observed in the far infrared range.[32] This measurement is consistent with Brown's estimate. Later observations in 2013 using combined thermal emission data from Herschel and the Spitzer Space Telescope suggested a smaller size of 1142+647
    −467     km     (710+402
    −290     mi    ), though this estimate had a larger range of uncertainty.[39]

    In 2016, combined observations from the Kepler spacecraft and archival thermal emission data from Herschel suggested that Gonggong was much larger than previously thought, giving a size estimate of 1535+75
    −225     km     (954+46
    −140     mi    ) based on an assumed equator-on view and a lower estimated albedo of 0.089.[9][10] This would have made Gonggong the third-largest trans-Neptunian object after Eris and Pluto, larger than Makemake (1,430 km (890 mi)).[10][22] These observations of Gonggong were part of the Kepler spacecraft's K2 mission which includes studying small Solar System bodies.[22] Subsequent measurements in 2018 revised the size of Gonggong to 1230±50 km (764±31 mi), based on the mass and density of Gonggong derived from the orbit of its satellite and the discovery that the viewing direction was almost pole-on.[8] With this size estimate, Gonggong is again thought to be the fifth-largest trans-Neptunian object.[8]

    Mass, density and rotation

    Based on the orbit of its satellite, the mass of Gonggong has been calculated to be 1.75×1021 kg (3.86×1021 lb), with a density of 1.72±0.16 g/cm3.[8] From these mass and density estimates, the size of Gonggong was calculated to be about 1,230 km (760 mi), smaller than the previous 2016 size estimate of 1,535 km (954 mi).[8] Given the mass, the 2016 size estimate of 1,535 km (954 mi) would have implied an unexpectedly low (and likely erroneous) density of 0.92 g/cm3.[8]

    Gonggong is the fifth most massive trans-Neptunian object, after Eris, Pluto, Haumea, and Makemake.[8] It is slightly more massive and denser than Charon, which has a mass of 1.586×1021 kg (3.497×1021 lb) and a density of 1.702 g/cm3.[8][45] Due to its large size, mass, and density, Gonggong is expected to be in hydrostatic equilibrium, taking the shape of a MacLaurin spheroid that is slightly flattened due to its rotation.[8][9]

    The rotation period of Gonggong was first measured in March 2016, through observations of variations in its brightness with the Kepler space telescope.[9] Gonggong's light curve amplitude as observed by Kepler is small, only varying in brightness by about 0.09 magnitudes.[9] The small light curve amplitude of Gonggong indicates that it is being viewed at a pole-on configuration, further evidenced by the observed inclined orbit of its satellite.[8] The Kepler observations provided ambiguous values of 44.81±0.37 and 22.4±0.18 hours for the rotation period.[9][8] Based on a best-fit model for its rotation pole orientation, the value of 22.4±0.18 hours is thought to be the more plausible one.[8] Gonggong rotates slowly compared to other trans-Neptunian objects, which usually have periods between 6 and 12 hours.[8] Due to its slow rotation, it is expected to have a low oblateness of 0.03 or 0.007, for rotation periods of 22.4 or 44.81 hours, respectively.[8]

    Orbit
    Polar view of the orbits of Gonggong, Eris, and Pluto
    Ecliptic view of the highly inclined orbits of Gonggong and Eris
    A preliminary motion analysis of Gonggong librating in a 3:10 resonance with Neptune. This animation consists of 16 frames covering 26,000 years.[5] Neptune (white dot) is held stationary.
    Apparent motion of Gonggong through the constellation Aquarius (years 2000 to 2050)

    Gonggong orbits the Sun at an average distance of 67.5 AU (1.010×1010 km; 6.27×109 mi), and completes a full orbit in 554 years.[3] The orbit of Gonggong is highly inclined to the ecliptic, with an orbital inclination 30.7 degrees.[3] Its orbit is also highly eccentric, with a measured orbital eccentricity of 0.50.[3] Due to its highly eccentric orbit, the distance of Gonggong from the Sun varies greatly over the course of its orbit, from 101.2 AU (1.514×1010 km; 9.41×109 mi) at aphelion, its furthest point from the Sun, to around 33.7 AU (5.04×109 km; 3.13×109 mi) at perihelion, its closest point to the Sun.[3][1] Gonggong reached perihelion in 1857, and is currently moving farther from the Sun, toward its aphelion.[46]

    The period, inclination and eccentricity of Gonggong's orbit are all rather extreme compared to other large bodies in the Solar system. Among likely dwarf planets, its period is the third longest, at 554 years compared to 558 years for Eris and the ca. 11,400 years of Sedna. Its 31° inclination is second, after 44° for Eris, and its 0.50 eccentricity is also (a rather distant) second, after Sedna at 0.84.

    The Minor Planet Center lists it as a scattered disc object for its eccentric and distant orbit.[4] The Deep Ecliptic Survey shows the orbit of Gonggong to be in a 3:10 resonance with Neptune; Gonggong completes three orbits around the Sun for every ten orbits completed by Neptune.[5]

    As of 2019, Gonggong is about 88 AU (1.32×1010 km; 8.2×109 mi) from the Sun[47] and is moving away at a speed of 1.1 kilometers per second (2,500 miles per hour).[48] It is the sixth-farthest known Solar System object from the Sun, preceding 2015 TH367 (89.5 AU), 2014 UZ224 (90.4 AU), Eris (96.1 AU), 2018 VG18 (~ 120 AU),[49] and "FarFarOut" (~ 140 AU).[47][50] Gonggong is more distant than Sedna, which is located 84.8 AU from the Sun as of July 2019.[47] It has been farther from the Sun than Sedna since 2013.[48] Gonggong will be farther than both Sedna and Eris by 2045,[51] and will reach aphelion by 2134.[13]

    Brightness

    Gonggong has an absolute magnitude (H) of 2.34,[11][9] which makes it the seventh-brightest trans-Neptunian object known. It is dimmer than Orcus (H=2.31; D=917 km)[52] but brighter than Quaoar (H=2.82; D=1,110 km).[53] The Minor Planet Center and the Jet Propulsion Laboratory Small-Body Database assume a brighter absolute magnitude of 1.6 and 1.8, respectively,[1][3] which would make it the fifth brightest trans-Neptunian object.[54]

    Being 88 AU from the Sun, the apparent magnitude of Gonggong is only 21.5,[55] and so it is too dim to be seen from Earth with the naked eye.[27][lower-alpha 5] Although closer to the Sun than the dwarf planet Eris, Gonggong appears dimmer, as Eris has a higher albedo and an apparent magnitude of 18.8.[32][57]

    Satellite
    Hubble images of Gonggong and Xiangliu, taken in 2009 and 2010 with the Wide Field Camera 3
    Main article: Xiangliu (moon)

    Following the March 2016 discovery that Gonggong was an unusually slow rotator, the possibility was raised that a satellite may have slowed it down via tidal forces.[58] The indications of a possible satellite orbiting Gonggong led Csaba Kiss and his team to analyze archival Hubble observations of Gonggong.[59] Their analysis of Hubble images taken on 18 September 2010 revealed a faint satellite orbiting Gonggong at a distance of at least 15,000 km (9,300 mi).[60] The discovery was announced in a Division for Planetary Sciences meeting on 17 October 2016.[27] The satellite is approximately 100 km (62 mi) in diameter and has an orbital period of 25 days.[59] On 5 February 2020 the satellite was officially named Xiangliu, after the nine-headed poisonous snake monster that accompanied Gonggong in Chinese mythology.[1]

    Exploration

    It was calculated by planetary scientist Amanda Zangari that a flyby mission to Gonggong would take a minimum of over 20 years with current rocket capabilities.[61] A flyby mission could take just under 25 years using a Jupiter gravity assist, based on a launch date of 2030 or 2031. Gonggong would be approximately 95 AU from the Sun when the spacecraft arrives.[61]

    See also

    Notes
    1. Discovery was announced two years later on 7 January 2009.
    2. In the convention for minor planet provisional designation, the first letter represents the half-month of the year of discovery while the second letter and numbers indicate the order of discovery within that half-month. In the case for 2007 OR10, the first letter 'O' corresponds to the second half-month of July 2007 while the last letter 'R' indicates that it is the 17th object discovered on the 11th cycle of discoveries. Each completed cycle consists of 25 letters representing discoveries, hence 17 + (10 completed cycles × 25 letters) = 267.[19]
    3. A larger magnitude value corresponds to a dimmer brightness and vice versa. The numerical value of Gonggong's absolute magnitude is 2.34,[9] hence it is dimmer than the IAU's minimum absolute magnitude of 1.
    4. The resulting minimum diameter of 580 km is derived from the equation , where is the absolute magnitude of Gonggong, and is the albedo of Gonggong, which in this case is assumed to be 1.[43]
    5. Under good conditions, the unaided human eye can detect objects with a visual magnitude of around +7.4 or lower.[56]

    References
    1. "(225088) Gonggong". Minor Planet Center. International Astronomical Union. Retrieved 2 November 2019.
    2. "MPEC 2009-A42 : 2007 OR10". Minor Planet Electronic Circular. Minor Planet Center. 7 January 2009. Retrieved 23 May 2019.
    3. "JPL Small-Body Database Browser: 225088 Gonggong (2007 OR10)" (2015-09-20 last obs.). Jet Propulsion Laboratory. 10 April 2017. Retrieved 20 February 2020.
    4. "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. International Astronomical Union. Retrieved 9 February 2018.
    5. Buie, M. W. (24 May 2019). "Orbit Fit and Astrometric record for 225088". Southwest Research Institute. Archived from the original on 24 May 2019.
    6. Johnston, W. R. (7 October 2018). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 23 May 2019.
    7. Brown, M. E. (20 May 2019). "How many dwarf planets are there in the outer solar system?". California Institute of Technology. Retrieved 23 May 2019.
    8. Kiss, C.; Marton, G.; Parker, A. H.; Grundy, W.; Farkas-Takacs, A.; Stansberry, J.; et al. (December 2019). "The mass and density of the dwarf planet (225088) 2007 OR10". Icarus. 334: 3–10. arXiv:1903.05439. Bibcode:2019Icar..334....3K. doi:10.1016/j.icarus.2019.03.013. S2CID 119370310.
      Initial publication at the American Astronomical Society DPS meeting #50, with the publication ID 311.02
    9. Pál, A.; Kiss, C.; Müller, T. G.; Molnár, L.; et al. (May 2016). "Large Size and Slow Rotation of the Trans-Neptunian Object (225088) 2007 OR10 Discovered from Herschel and K2 Observations". The Astronomical Journal. 151 (5): 8. arXiv:1603.03090. Bibcode:2016AJ....151..117P. doi:10.3847/0004-6256/151/5/117. S2CID 119205487.
    10. Szabó, R. (4 November 2015). "Pushing the Limits of K2: Observing Trans-Neptunian Objects S3K2: Solar System Studies with K2" (PDF). Archived from the original (PDF) on 7 February 2019.
    11. Boehnhardt, H.; Schulz, D.; Protopapa, S.; Götz, C. (November 2014). "Photometry of Transneptunian Objects for the Herschel Key Program 'TNOs are Cool'". Earth, Moon, and Planets. 114 (1–2): 35–57. Bibcode:2014EM&P..114...35B. doi:10.1007/s11038-014-9450-x. S2CID 122628169.
    12. "LCDB Data for (225088)". Asteroid Lightcurve Database (LCDB). Retrieved 14 May 2019.
    13. Grundy, Will (13 February 2020). "Gonggong (225088 2007 OR10)". Lowell Observatory. Archived from the original on 20 February 2020. Retrieved 19 February 2020.
    14. Schwamb, M. E.; Brown, M. E.; Rabinowitz, D. L. (March 2009). "A Search for Distant Solar System Bodies in the Region of Sedna". The Astrophysical Journal Letters. 694 (1): L45–L48. arXiv:0901.4173. Bibcode:2009ApJ...694L..45S. doi:10.1088/0004-637X/694/1/L45. S2CID 15072103.
    15. Schwamb, M. (9 April 2019). "2007 OR10 Needs a Name!". The Planetary Society. Archived from the original on 24 May 2019. Retrieved 24 May 2019.
    16. Schwamb, M. E.; Brown, M. E.; Rabinowitz, D. L.; Ragozzine, D. (25 August 2010). "Properties of the Distant Kuiper Belt: Results from the Palomar Distant Solar System Survey". The Astrophysical Journal Letters. 720 (2): 1691–1707. arXiv:1007.2954. Bibcode:2010ApJ...720.1691S. doi:10.1088/0004-637X/720/2/1691. S2CID 5853566.
    17. Brown, M. E. (29 November 2010). "There's something out there -- part 3". Mike Brown's Planets. Retrieved 10 May 2019.
    18. "Astronomers Find Ice and Possibly Methane On Snow White, a Distant Dwarf Planet". Science Daily. California Institute of Technology. 22 August 2011. Retrieved 5 March 2018.
    19. "New- And Old-Style Minor Planet Designations". Minor Planet Center. International Astronomical Union. Retrieved 10 May 2019.
    20. Lowe, A. "(225088) 2007 OR10 Precovery Images". Andrew Lowe's Minor Planet Home Page. Retrieved 6 May 2019.
    21. Schwamb, M. (29 May 2019). "The People Have Voted on 2007 OR10's Future Name!". The Planetary Society. Retrieved 29 May 2019.
    22. Dyches, P. (11 May 2016). "2007 OR10: Largest Unnamed World in the Solar System". Jet Propulsion Laboratory. Retrieved 12 May 2016.
    23. Brown, M. E. (9 August 2011). "The Redemption of Snow White (Part 1)". Mike Brown's Planets.
    24. Brown, M. E. (10 March 2009). "Snow White needs a bailout". Mike Brown's Planets. Archived from the original on 17 May 2009. Retrieved 17 February 2010.
    25. Williams, M. (3 September 2015). "The (possible) dwarf planet 2007 OR10". Universe Today. Retrieved 2 November 2019.
    26. Plotner, T. (3 August 2011). ""Snow White" or "Rose Red" (2007 OR10)". Universe Today. Retrieved 8 May 2019.
    27. Schwamb, M.; Brown, M. E.; Rabinowitz, D. L. "Help Name 2007 OR10". Archived from the original on 25 May 2019. Retrieved 9 April 2019.
    28. "How Are Minor Planets Named?". Minor Planet Center. International Astronomical Union. Retrieved 8 May 2019.
    29. "Astronomers Invite the Public to Help Name Kuiper Belt Object". International Astronomical Union. 10 April 2019. Retrieved 12 May 2019.
    30. "M.P.C. 121135" (PDF). Minor Planet Circular. Minor Planet Center. 5 February 2020. Retrieved 19 February 2020.
    31. Brown, M. E. (May 2012). "The compositions of Kuiper belt objects" (PDF). Annual Review of Earth and Planetary Sciences. 40 (1): 467–494. arXiv:1112.2764. Bibcode:2012AREPS..40..467B. doi:10.1146/annurev-earth-042711-105352. S2CID 14936224. Retrieved 19 May 2019.
    32. Santos-Sanz, P.; Lellouch, E.; Fornasier, S.; Kiss, C.; et al. (May 2012). ""TNOs are Cool": A survey of the trans-Neptunian region. IV. Size/albedo characterization of 15 scattered disk and detached objects observed with Herschel-PACS". Astronomy & Astrophysics. 541 (A92): 18. arXiv:1202.1481. Bibcode:2012A&A...541A..92S. doi:10.1051/0004-6361/201118541. S2CID 118600525.
    33. Brown, M. E.; Burgasser, A. J.; Fraser, W. C. (September 2011). "The Surface Composition of Large Kuiper Belt Object 2007 OR10" (PDF). The Astrophysical Journal Letters. 738 (2): 4. arXiv:1108.1418. Bibcode:2011ApJ...738L..26B. doi:10.1088/2041-8205/738/2/L26. hdl:1721.1/95722. S2CID 9730804.
    34. Brown, M. E.; Schaller, E. L.; Fraser, W. C. (May 2012). "The compositions of Kuiper belt objects" (PDF). The Astrophysical Journal. 143 (6): 146. arXiv:1204.3638. doi:10.1088/0004-6256/143/6/146. S2CID 8886741. Retrieved 19 May 2019.
    35. Brown, M. E. (20 August 2011). "The Redemption of Snow White (Part 3 of 3)". Mike Brown's Planets. Archived from the original on 25 July 2014.
    36. Holler, B. J.; Young, L. A.; Bus, S. J.; Protopapa, S. (September 2017). Methanol ice on Kuiper Belt objects 2007 OR10 and Salacia: Implications for formation and dynamical evolution (PDF). European Planetary Science Congress 2017. 11. European Planetary Science Congress. Bibcode:2017EPSC...11..330H. EPSC2017-330.
    37. Johnson, R. E.; Oza, A.; Young, L. A.; Volkov, A. N.; Schmidt, C. (August 2015). "Volatile Loss and Classification of Kuiper Belt Objects". The Astrophysical Journal. 809 (1): 43. arXiv:1503.05315. Bibcode:2015ApJ...809...43J. doi:10.1088/0004-637X/809/1/43. S2CID 118645881.
    38. Tancredi, G. (6 April 2010). "Physical and dynamical characteristics of icy "dwarf planets" (plutoids)". Proceedings of the International Astronomical Union. 5 (S263): 173–185. Bibcode:2010IAUS..263..173T. doi:10.1017/S1743921310001717. Retrieved 14 May 2019.
    39. Lellouch, E.; Santos-Sanz, P.; Lacerda, P.; Mommert, M.; et al. (August 2013). ""TNOs are Cool": A survey of the trans-Neptunian region. IX. Thermal properties of Kuiper belt objects and Centaurs from combined Herschel and Spitzer observations" (PDF). Astronomy & Astrophysics. 557 (A60): 19. arXiv:1202.3657. Bibcode:2013A&A...557A..60L. doi:10.1051/0004-6361/201322047.
    40. "Naming of Astronomical Objects". International Astronomical Union. Retrieved 2 November 2019.
    41. "IAU 2006 General Assembly: Result of the IAU Resolution votes" (Press release). International Astronomical Union. 24 August 2006. Retrieved 2 October 2019.
    42. Sheppard, S. S.; Udalski, A.; Trujillo, Ch.; Kubiak, M.; et al. (October 2011). "A Southern Sky and Galactic Plane Survey for Bright Kuiper Belt Objects". The Astronomical Journal. 142 (4): 10. arXiv:1107.5309. Bibcode:2011AJ....142...98S. doi:10.1088/0004-6256/142/4/98. S2CID 53552519.
    43. Bruton, D. "Conversion of Absolute Magnitude to Diameter for Minor Planets". Department of Physics, Engineering, and Astronomy. Stephen F. Austin State University. Retrieved 14 May 2019.
    44. 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.
    45. Stern, S. A.; Grundy, W.; McKinnon, W. B.; Weaver, H. A.; Young, L. A. (September 2018). "The Pluto System After New Horizons". Annual Review of Astronomy and Astrophysics. 56: 357–392. arXiv:1712.05669. Bibcode:2018ARA&A..56..357S. doi:10.1146/annurev-astro-081817-051935. S2CID 119072504.
    46. "Asteroid 2007 OR10". The Sky Live. Retrieved 7 May 2019.
    47. "AstDyS-2, Asteroids - Dynamic Site". Asteroids Dynamic Site. Department of Mathematics, University of Pisa. Retrieved 3 July 2019. Objects with distance from Sun over 84.2 AU
    48. "Horizon Online Ephemeris System" (Settings: Ephemeris Type "VECTORS", Table Settings "output units=KM-S"). Jet Propulsion Laboratory. Retrieved 2 November 2019.
    49. "Discovered: The Most-Distant Solar System Object Ever Observed". Carnegie Science. 17 December 2018. Retrieved 7 May 2019.
    50. Voosen, P. (21 February 2019). "Astronomers Discover Solar System's Most Distant Object, Nicknamed 'FarFarOut'". Science. doi:10.1126/science.aax1154.
    51. "Horizons Output for Sedna 2076/2114". 17 February 2011. Archived from the original on 25 February 2012. Retrieved 17 February 2011.
    52. Fornasier, S.; Lellouch, E.; Müller, T.; Santos-Sanz, P.; et al. (July 2013). "TNOs are Cool: A survey of the trans-Neptunian region. VIII. Combined Herschel PACS and SPIRE observations of 9 bright targets at 70–500 µm". Astronomy & Astrophysics. 555 (A15): 22. arXiv:1305.0449v2. Bibcode:2013A&A...555A..15F. doi:10.1051/0004-6361/201321329.
    53. Braga-Ribas, F.; Sicardy, B.; Ortiz, J. L.; Lellouch, E.; et al. (August 2013). "The Size, Shape, Albedo, Density, and Atmospheric Limit of Transneptunian Object (50000) Quaoar from Multi-chord Stellar Occultations". The Astrophysical Journal. 773 (1): 13. Bibcode:2013ApJ...773...26B. doi:10.1088/0004-637X/773/1/26. hdl:11336/1641.
    54. Brown, M. E. (11 August 2011). "The Redemption of Snow White (Part 2 of 3)". Mike Brown's Planets. Archived from the original on 25 July 2014.
    55. "(225088) Gonggong Observation Prediction". Asteroids Dynamic Site. Department of Mathematics, University of Pisa, Italy. Archived from the original on 24 May 2019. Retrieved 24 May 2019.
    56. Sinnott, Roger W. (19 July 2006). "What's my naked-eye magnitude limit?". Sky and Telescope. Retrieved 17 April 2019.
    57. "(136199) Eris Observation prediction". Asteroids Dynamic Site. Department of Mathematics, University of Pisa, Italy. Archived from the original on 24 May 2019. Retrieved 2 November 2019.
    58. Lakdawalla, E. (19 October 2016). "DPS/EPSC update: 2007 OR10 has a moon!". The Planetary Society. Retrieved 19 October 2016.
    59. Kiss, C.; Marton, G.; Farkas-Takács, A.; Stansberry, J.; et al. (March 2017). "Discovery of a Satellite of the Large Trans-Neptunian Object (225088) 2007 OR10". The Astrophysical Journal Letters. 838 (1): L1. arXiv:1703.01407. Bibcode:2017ApJ...838L...1K. doi:10.3847/2041-8213/aa6484. S2CID 46766640.
    60. Marton, G.; Kiss, C.; Mueller, T. G. (October 2016). "The moon of the large Kuiper-belt object 2007 OR10" (PDF). Division for Planetary Sciences Abstract Book. DPS 48/EPSC 11 Meeting. 48. American Astronomical Society. 120.22. Retrieved 24 May 2019.
    61. Zangari, A. M.; Finley, T. J.; Stern, S. A.; Tapley, M. B. (May 2019). "Return to the Kuiper Belt: Launch Opportunities from 2025 to 2040". Journal of Spacecraft and Rockets. 56 (3): 919–930. arXiv:1810.07811. Bibcode:2019JSpRo..56..919Z. doi:10.2514/1.A34329. S2CID 119033012.

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