(55636) 2002 TX300

Haumea family Kuiper belt object April 2020 yes #C2E0FF (55636) 2002 TX 300 2002 TX300 Hubble 8x upscale.png 2002 TX 300 imaged by the Hubble Space Telescope on 16 September 2005 NEAT Palomar Obs. 15 October 2002 (55636) 2002 TX 300 TNO classical (hot) Haumea family distant Scat-Ext barycentric 5 May 2025 (JD 2460800.5) 0 70+ yr 27 August 1954 yes 48.587 AU 37.919 AU ≈ 24 June 2242barycentric 43.253 AU 0.1233 284.28 yr (103,832 d) 84.179° 0.0034671 ms / day 25.853° 324.578° 340.302° 0 320 50 km (2019) 323 95 37 km (2018)7 ≈1.1 19 kg (est. water ice density)899 ≈1 g/cm3 (assumed water ice)8999 8.04 0.04 h (single-peaked)rotation or 16.08 0.04 h (double-peaked)rotation 0.65 0.15 (2020) 0.76 +0.18 -0.45 (2018)7 BBb (neutral)The trans-Neptunian object spectral type "BBb" indicates the object has both a "spectrally neutral" color (BB) and a high albedo (b).1826 B–V 0.70 0.0928 V–R 0.36 0.0228 V–I 0.68 0.1228 3.574 0.05513 3.51 (JPL) 19 to 20 5 milliarcseconds8 49 K (subsolar)899 (55636) 2002 TX 300 is an icy trans-Neptunian object orbiting the Sun in the Kuiper belt. It has a diameter of about 300 km mi and a highly reflective surface made of fresh water ice. It is the brightest and possibly the largest known member of the Haumea family,4, 8559 a population of Kuiper belt objects that broke off from the dwarf planet Haumea 4.4 billion years ago. 2002 TX 300 was discovered on 15 October 2002 by the NASA-directed Near-Earth Asteroid Tracking (NEAT) survey at Palomar Observatory. When it was discovered, astronomers initially inferred from its high brightness that it could be a large dwarf planet almost 1000 km mi in diameter. This was later disproven in October 2009, when astronomers measured the diameter of 2002 TX 300 for the first time by observing the object occulting or blocking out the light of a background star. 2002 TX 300 is now known to be too small to likely qualify as a dwarf planet, and its brightness mainly comes from its reflective surface. 2002 TX 300 was the first Kuiper belt object (besides Pluto and its moon Charon) that was observed via stellar occultation.2 History Discovery 2002 TX 300 was discovered on 15 October 2002 by the Near-Earth Asteroid Tracking (NEAT) survey, which was a NASA-directed project for finding near-Earth asteroids in the sky using telescopes at various observatories across the United States. The telescope that discovered 2002 TX 300 was the 1.22 m in on us Samuel Oschin telescope at Palomar Observatory in San Diego County, California. The people involved in making the discovery observations at Palomar included Eleanor Helin, Steven Pravdo, Kenneth Lawrence, Michael D. Hicks, and R. Thicksten. Additional confirming observations were provided by Powell Observatory, Table Mountain Observatory, and Stephen P. Laurie at Church Stretton (obs. code 966) during the three days following the discovery of 2002 TX 300. The Minor Planet Center (MPC) announced the discovery of 2002 TX 300 on 22 Oct 2002. Within a day after the announcement, astronomer Reiner Stoss found pre-discovery observations of 2002 TX 300 in NEAT images from 2001 to 2002 and Digitized Sky Survey images from 1954 to 1995. The earliest known pre-discovery observation of 2002 TX 300 came from Siding Spring Observatory images taken on 27 August 1954. horizontal center 500 P48 1994 Jean Large.jpg 2002 TX300 discovery annotated crop.gif The 1.2-meter Samuel Oschin telescope that discovered 2002 TX 300 at Palomar Observatory Discovery images of 2002 TX 300 from 15 October 2002 Number and name This object has the minor planet provisional designation 2002 TX 300, which was given by the MPC in the discovery announcement. The provisional designation indicates the year and half-month of the object's discovery date. 2002 TX 300 received its permanent minor planet catalog number of 55636 from the MPC on 16 February 2003. The Kuiper belt objects 55637 Uni and (55638) 2002 VE 95 directly come after (55636) 2002 TX 300's number in the minor planet catalog. 2002 TX 300 does not have a proper name and the discoverers' privilege for naming this object expired ten years after it was numbered.6 According to naming guidelines by the International Astronomical Union's Working Group for Small Bodies Nomenclature, 2002 TX 300 is open for name suggestions that relate to creation myths, as recommended for Kuiper belt objects in general.8 Orbit and classification thumb|left|upright=1.5|Diagram showing an oblique view of the orbits of 2002 TX 300 (white), Haumea (pink), and the planets. Rows of dark vertical lines along the inclined orbits of 2002 TX 300 and Haumea indicate their vertical distances above or below the ecliptic plane. 2002 TX 300 is a trans-Neptunian object (TNO) orbiting the Sun at a semi-major axis or average distance of 43.3 astronomical units (AU).barycentric These orbital elements are expressed in terms of the Solar System Barycenter (SSB) as the frame of reference. Due to planetary perturbations, the Sun revolves around the SSB at non-negligible distances, so heliocentric-frame orbital elements and distances can vary in short timescales as shown in JPL-Horizons. It follows an elliptical orbit that has an eccentricity of 0.12 and a high inclination2537 of 25.9° with respect to the ecliptic. In its 284-year-long orbit, 2002 TX 30 comes as close as 37.9 AU from the Sun at perihelion and as far as 48.6 AU from the Sun at aphelion. 2002 TX 300 last passed perihelion in February 1952 and will make its next perihelion passage on 24 June 2242. 2002 TX 300 is located in the classical region of the Kuiper belt 39–48 AU from the Sun,53 and is thus classified as a classical Kuiper belt object (sometimes known as a "cubewano").55 The high orbital inclination of 2002 TX 300 makes it a dynamically "hot" member of the classical Kuiper belt, which implies that it was gravitationally scattered out to its present location by Neptune's outward planetary migration in the Solar System's early history.230 Because of this, 2002 TX 300 has sometimes been classified as a "scattered" object.187165 Haumea family 400px|thumb|A chart showing confirmedModeling the Formation of the Family of the Dwarf Planet Haumea Benjamin Proudfoot Darin Ragozzine The Astronomical Journal May 2019 157 6 230 1904.00038 10.3847/1538-3881/ab19c4 2019AJ....157..230P 90262136 freeA Near-infrared Survey of Candidate Haumea Family Members Benjamin Proudfoot Estela Fernández-Valenzuela John Stansberry Csaba Kiss Darin Ragozzine Wesley Fraser Rosemary Pike Noemi Pinilla-Alonso The Astronomical Journal December 2024 168 6 269 10.3847/1538-3881/ad864e 2024AJ....168..269P 274155364 free 10831/121057 free Haumea family members to scale (2025 y). Unmeasured members are shown with estimated diameters using an assumed albedo of 0.7. Haumea family The orbit of 2002 TX 300 is very similar to that of the dwarf planet Haumea, which suggests that 2002 TX 300 could be a collisional fragment of the dwarf planet. 2002 TX 300's surface color, composition, and reflectivity matches that of Haumea as well, which lends further credibility to this scenario. It is now widely accepted among researchers that 2002 TX 300 originated from Haumea; it is classified as a member of the Haumea family, a population of Kuiper belt objects that are suspected to be fragments of Haumea. Physical characteristics Surface and composition The surface of 2002 TX 300 is mostly made of highly reflective fresh water ice, which makes the object appear bright and "spectrally neutral" in visible light8—meaning it reflects equal amounts of light across the visible spectrum, which gives 2002 TX 300 a gray color. With a geometric albedo between 50% and 80%,The 50%–80% range (also written as 0.5–0.8 in decimal form) is the lower and upper bound for the albedo value of 0.65 0.15 given by Ortiz et al. (2019). 2002 TX 300 has one of the most reflective surfaces seen among Kuiper belt objects (KBOs).14 2002 TX 300 stands out from typical KBOs, whose surfaces are commonly dark and reddened due to irradiated organic compounds or tholins.8 The object's spectrum in the visible and near-infrared ranges is very similar to that of Charon, characterized by neutral to blue slope (1%/1000 Å) with deep (60%) water absorption bands at 1.5 and 2.0 μm. Mineralogical analysis indicates a substantial fraction of large ice (H2O) particles. The signal-to-noise ratio of the observations was insufficient to differentiate between amorphous or crystalline ice (crystalline ice was reported on Charon, Quaoar and Haumea). The proportion of highly processed organic materials (tholins), typically present on numerous trans-Neptunian objects, is very low. As suggested by Licandro et al. 2006, this lack of irradiated mantle suggest either a recent collision or comet activity. Size thumb|This graphic used in the first draft of the 2006 IAU planet definition suggested that 2002 TX 300 could be as large as the dwarf planet Quaoar.17 2002 TX 300 has a diameter of 320 ± 50 km mi, according to measurements from stellar occultation observations. At this size, 2002 TX 300 is too small to gravitationally collapse itself into a sphere (be in hydrostatic equilibrium),9 so it does not qualify as a dwarf planet.243 For comparison, the diameter of Saturn's smallest round moon Mimas is 396 km mi. Although the mass and density of 2002 TX 300 have not been measured, its overall composition has been inferred to be mostly water ice like its surface, which would suggest that 2002 TX 300's bulk density should be likely around 1 g/cm3, similar to that of water ice.8999 This density would correspond to a mass on the order of 19 kg (about 1.6 -4 times the mass of Earth's Moon) for 2002 TX 300.899 History of size estimates + History of diameter estimates for 2002 TX 300Year ofPublicationDiameter(km)MethodRefs2005≤709thermal(IRAM)1872008<641.2 +250.3 -206.7thermal(Spitzer)1732009<420thermal(Spitzer, remodeled)2912010286 10occultation2018323 +95 -37occultation(reanalyzed)72020320 50occultation(reanalyzed) When 2002 TX 300 was discovered, astronomers initially thought it could be a large dwarf planet up to 1000 km mi in diameter,1321178 because it was one of the brightest KBOs known at the time. 2002 TX 300 was even included in the International Astronomical Union's (IAU) roster of dwarf planet candidates in their first draft of the 2006 IAU definition of "planet", where they cited an upper limit diameter of 700 km mi for 2002 TX 300.1750 This overestimation of 2002 TX 300's diameter came from astronomers incorrectly assuming that it has a dark, low-albedo surface like the bright KBOs 50000 Quaoar, 55565 Aya, and 20000 Varuna.387–388 Astronomers began suspecting that 2002 TX 300 must be smaller than initially thought, when far-infrared and radio telescopes showed no significant thermal emission coming from the object.1871739 Astronomers were able to measure the diameter and albedo of 2002 TX 300 for the first time on 9 October 2009, when the object occulted or blocked out the light of a background star. 2002 TX 300 was the first Kuiper belt object (besides Pluto and its moon Charon) that was observed via stellar occultation.2 The stellar occultation was predicted and observed by a network of astronomers stationed at 18 different locations across Hawaii.897 Only two of these locations successfully observed the occultation; an initial analysis of their detections indicated that 2002 TX 300 should have a diameter of 286 km mi if it was spherical.898 However, this diameter estimate was affected by a timing error between the two occultation detections; reanalysis of the 2009 occultation data in 2018 and 2019 suggested that 2002 TX 300 should have a slightly larger diameter of about 320 km mi.9 Shape and rotation Although the exact shape of 2002 TX 300 is unknown, it is expected to be similar to an oblate spheroid, with irregularities.9 Observations of 2002 TX 300's brightness over time indicate it has a rotation period of either 8.04 or 16.08 hours, depending on whether the object's brightness variability is caused by surface albedo variations or an elongated shape.rotation The rotation period of 2002 TX 300 was measured by observing how its brightness changes over time, which is plotted as a light curve. If 2002 TX 300 has a spheroidal shape, then its light curve should resemble a "single-peaked" sine wave, whereas if 2002 TX 300 is elongated, then its light curve should resemble a "double-peaked" sine wave.25392537, 2542 Studies from 2003 to 2018 have consistently shown that 2002 TX 300 exhibits very little brightness variation (less than 0.1 magnitudes),2539 which makes it difficult to determine its rotation period.316113 The axial tilt of 2002 TX 300 is unknown.386 Lack of atmosphere Observations of the 9 October 2009 stellar occultation by 2002 TX 300 showed that the object lacks an atmosphere with a surface number density greater than 2 15 particles per cubic centimetre.899 2002 TX 300 is expected to not have an atmosphere because its mass is too small for its gravity to hold onto light gases.899 See also (19308) 1996 TO 66 – the first Haumea family member discovered Notes References 30em 2025-01-02 last obs. JPL Small-Body Database Lookup: 55636 (2002 TX300) https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/?sstr=20055636 Jet Propulsion Laboratory 2025-07-18 (55636) = 2002 TX300 https://www.minorplanetcenter.net/db_search/show_object?object_id=55636 Minor Planet Center 2025-07-18 JPL Horizons On-Line Ephemeris for 55636 (2002 TX300) at epoch JD 2460800.5 https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND='55636'&TABLE_TYPE='ELEMENTS'&START_TIME='JD2460800.5'&STOP_TIME='JD2460801.5'&STEP_SIZE='1y'&CENTER='@0'&OUT_UNITS='AU-D' JPL Horizons On-Line Ephemeris System Jet Propulsion Laboratory 2025-07-18 Solution using the Solar System Barycenter. Ephemeris Type: Elements and Center: @0) JPL Horizons On-Line Ephemeris for 55636 (2002 TX300) at epochs JD 2460800.5–2461000.5 https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND='55636'&TABLE_TYPE='ELEMENTS'&START_TIME='JD2460800.5'&STOP_TIME='JD2461000.5'&STEP_SIZE='200d'&CENTER='500@10'&OUT_UNITS='AU-D' JPL Horizons On-Line Ephemeris System Jet Propulsion Laboratory 2025-07-18 Solution using the Sun. Ephemeris Type: Elements and Center: @sun) JPL Horizons On-Line Ephemeris for 55636 (2002 TX300) from 1958-Feb-01 to 1958-Feb-20 https://ssd.jpl.nasa.gov/api/horizons.api?format=text&COMMAND=%2755636%27&OBJ_DATA=%27YES%27&MAKE_EPHEM=%27YES%27&EPHEM_TYPE=%27OBSERVER%27&CENTER=%27@sun%27&START_TIME=%271958-02-01%27&STOP_TIME=%271958-02-20%27&STEP_SIZE=%271d%27&QUANTITIES=%2720%27 JPL Horizons On-Line Ephemeris System Jet Propulsion Laboratory 2025-07-19 (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 1-sigma from JPL Small-Body Database.) JPL Horizons On-Line Ephemeris for 55636 (2002 TX300) from 2242-Jun-01 to 2242-Jun-30 https://ssd.jpl.nasa.gov/api/horizons.api?format=text&COMMAND=%2755636%27&OBJ_DATA=%27YES%27&MAKE_EPHEM=%27YES%27&EPHEM_TYPE=%27OBSERVER%27&CENTER=%27@sun%27&START_TIME=%272242-06-01%27&STOP_TIME=%272242-06-30%27&STEP_SIZE=%271d%27&QUANTITIES=%2720%27 JPL Horizons On-Line Ephemeris System Jet Propulsion Laboratory 2025-07-19 (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 1-sigma from JPL Small-Body Database.) Orbit Fit and Astrometric record for 55636 http://www.boulder.swri.edu/~buie/kbo/astrom/55636.html Marc W. Buie Southwest Research Institute 2025-07-18 live https://web.archive.org/web/20241125231423/https://www.boulder.swri.edu/~buie/kbo/astrom/55636.html 2024-11-25 M.P.C. 47763 https://minorplanetcenter.net/iau/ECS/MPCArchive/2003/MPC_20030216.pdf#page=325 Minor Planet Circulars Minor Planet Center 47763 325 2003-02-16 2025-07-18 New- And Old-Style Minor Planet Designations https://www.minorplanetcenter.net/iau/info/DesDoc.html Minor Planet Center 2025-07-15 Rules and Guidelines for Naming Non-Cometary Small Solar-System Bodies https://www.wgsbn-iau.org/documentation/NamesAndCitations.pdf IAU Working Group for Small Bodies Nomenclature 22 February 2025 19 June 2025 Planetary Satellite Physical Parameters https://ssd.jpl.nasa.gov/sats/phys_par/sep.html Jet Propulsion Laboratory 2025-07-19 etal E. F. Helin S. Pravdo K. Lawrence M. Hicks R. Thicksten M. Glaze MPEC 2002-U17 : 2002 TX300 https://www.minorplanetcenter.net/iau/mpec/K02/K02U17.html Minor Planet Electronic Circular Minor Planet Center 22 October 2002 2002-U17 2025-07-18 2002MPEC....U...17H etal R. Stoss E. F. Helin S. Pravdo K. Lawrence M. Hicks R. Thicksten MPEC 2002-U19 : 2002 TX300 https://www.minorplanetcenter.net/iau/mpec/K02/K02U19.html Minor Planet Electronic Circular Minor Planet Center 22 October 2002 2002-U19 2025-07-18 2002MPEC....U...19S Raymond J. Bambery Eleanor F. Helin Steven H. Pravdo Kenneth J. Lawrence Michael D. Hicks An update of the Near-Earth Asteroid Tracking/Maui Space Surveillance System (NEAT/MSSS) collaboration https://dataverse.jpl.nasa.gov/file.xhtml?fileId=42940&version=2.0 2002 AMOS Technical Conference Maui, Hawaii September 2002 131088143 2014/11237 etal J. L. Ortiz A. Sota E. Moreno W. Lellouch N. Biver A. Doressoundiram A study of Trans-Neptunian object (55636) 2002 TX 300 Astronomy & Astrophysics June 2004 420 383–388 free 10.1051/0004-6361:20034507 2004A&A...420..383O 55594911 W. M. Grundy K. S. Noll D. C. Stephens Diverse albedos of small trans-neptunian objects Icarus July 2005 176 1 184–191 10.1016/j.icarus.2005.01.007 2005Icar..176..184G astro-ph/0502229 118866288 Patryk Sofia Lykawka Mukai Tadashi Higher albedos and size distribution of large transneptunian objects Planetary and Space Science November 2005 53 13 1319–1330 10.1016/j.pss.2005.06.004 2005P&SS...53.1319L 123571645 O. Gingerich Owen Gingerich Planet Definition Q & A Factsheet https://www.iau.org/static/publications/ga_newspapers/20060812.pdf#page=17 Dissertatio CVM Nvncio Sidereo III International Astronomical Union 12 August 2006 3 17 13 March 2007 dead https://web.archive.org/web/20150315084508/http://www.iau.org/static/publications/ga_newspapers/20060812.pdf 15 March 2015 Lars Lindberg Christensen Helen Sim Raquel Yumi Shida Nadja Wolf Lars Holm Nielsen The public communication at the IAU GA 2006 https://www.iau.org/static/public_press/iau_po_report.pdf#page=50 IAU XXVIth General Assembly International Astronomical Union 2006 26 50 29 March 2025 dead https://web.archive.org/web/20130501174441/https://www.iau.org/static/public_press/iau_po_report.pdf#page=50 1 May 2013 Patryk Sofia Lykawka Mukai Tadashi Dynamical classification of trans-neptunian objects: Probing their origin, evolution, and interrelation Icarus July 2007 189 1 213–232 10.1016/j.icarus.2007.01.001 2007Icar..189..213L 122671996 Brett Gladman Brian G. Marsden Christa VanLaerhoven Nomenclature in the Outer Solar System https://www.lpi.usra.edu/books/ssbn2008/7002.pdf The Solar System Beyond Neptune University of Arizona Press 2008 43–57 9780816527557 astro-ph/0702538 2008ssbn.book...43G 14469199 dead https://web.archive.org/web/20230801104434/https://www.lpi.usra.edu/books/ssbn2008/7002.pdf 1 August 2023 Alain Doressoundiram Hermann Boehnhardt Stephen C. Tegler Chad Trujillo Color Properties and Trends of the Transneptunian Objects https://scispace.com/pdf/color-properties-and-trends-of-the-transneptunian-objects-2q399gmus5.pdf The Solar System Beyond Neptune University of Arizona Press 2008 91–104 9780816527557 2008ssbn.book...91D 55188715 live https://web.archive.org/web/20141209052738/http://www.lpi.usra.edu/books/ssbn2008/7016.pdf 9 December 2014 Marcello Fulchignoni Irina Belskaya Maria Antonietta Barucci Maria Cristina De Sanctis Alain Doressoundiram Transneptunian Object Taxonomy https://web.gps.caltech.edu/~mbrown/out/kbbook/Chapters/Fulchignoni_Taxonomy.pdf The Solar System Beyond Neptune University of Arizona Press 2008 181–192 9780816527557 2008ssbn.book..181F 54970643 John Stansberry Will Grundy Mike Brown Dale Cruikshank John Spencer David Trilling Jean-Luc Margot Physical Properties of Kuiper Belt and Centaur Objects: Constraints from the Spitzer Space Telescope https://web.gps.caltech.edu/~mbrown/out/kbbook/Chapters/Stansberry_Spitzer.pdf The Solar System Beyond Neptune University of Arizona Press 2008 161–179 9780816527557 astro-ph/0702538 2008ssbn.book..161S 578439 David L. Rabinowitz Bradley E. Schaefer Martha W. Schaefer Suzanne W. Tourtellotte The Youthful Appearance of the 2003 EL61 Collisional Family The Astronomical Journal October 2008 136 4 1502–1509 free 10.1088/0004-6256/136/4/1502 0804.2864 2008AJ....136.1502R 117167835 M. J. Brucker W. M. Grundy J. A. Stansberry J. R. Spencer S. S. Sheppard E. I. Chiang M. W. Buie High albedos of low inclination Classical Kuiper belt objects Icarus May 2009 201 1 284–294 10.1016/j.icarus.2008.12.040 0812.4290 2009Icar..201..284B 53543791 Gonzalo Tancredi Physical and dynamical characteristics of icy "dwarf planets" (plutoids) Proceedings of the International Astronomical Union 6 April 2010 5 S263 173–185 free 10.1017/S1743921310001717 2010IAUS..263..173T etal J. L. Elliot M. J. Person C. A. Zuluaga A. S. Bosh E. R. Adams T. C. Brothers Size and albedo of Kuiper belt object 55636 from a stellar occultation https://apps.dtic.mil/sti/tr/pdf/ADA541934.pdf Nature June 2010 465 7300 897–900 10.1038/nature09109 2010Natur.465..897E 20559381 4431420 dead https://web.archive.org/web/20140222100203/http://www.dtic.mil/cgi-bin/GetTRDoc?AD=ADA541934&Location=U2&doc=GetTRDoc.pdf 2014-02-22 etal J. L. Elliot M. J. Person C. A. Zuluaga A. S. Bosh E. R. Adams T. C. Brothers Size and Albedo of the Kuiper Belt Object 55636 AAS Division for Planetary Sciences meeting #42 American Astronomical Society 23.02 October 2010 2010DPS....42.2302E etal M. Assafin J. I. B. Camargo R. Vieira Martins F. Braga-Ribas B. Sicardy A. H. Andrei Candidate stellar occultations by large trans-Neptunian objects up to 2015 Astronomy & Astrophysics May 2012 541 A142 A142 free 10.1051/0004-6361/201118349 1204.4234 2012A&A...541A.142A 119113077 etal A. Thirouin J. L. Ortiz A. Campo Bagatin P. Pravec N. Morales O. Hainaut Short-term variability of 10 trans-Neptunian objects Monthly Notices of the Royal Astronomical Society August 2012 424 4 3156–3177 free 10.1111/j.1365-2966.2012.21477.x 1207.2044 2012MNRAS.424.3156T 53467482 etal F. Braga-Ribas B. Sicardy J. L. Ortiz E. Lellouch G. Tancredi J. Lecacheux The Size, Shape, Albedo, Density, and Atmospheric Limit of Transneptunian Object (50000) Quaoar from Multi-chord Stellar Occultations The Astrophysical Journal August 2013 773 1 10.1088/0004-637X/773/1/26 2013ApJ...773...26B 11336/1641 53724395 https://orbi.uliege.be/handle/2268/156970 free 29 April 2021 21 April 2022 https://web.archive.org/web/20220421180714/https://orbi.uliege.be/handle/2268/156970 live Noemi Pinilla-Alonso Icy Dwarf Planets: Colored Popsicles in the Outer Solar System Proceedings of the International Astronomical Union August 2015 11 A29A 241–246 free 10.1017/S1743921316002970 2016IAUFM..29A.241P etal A. Alvarez-Candal N. Pinilla-Alonso J. L. Ortiz R. Duffard N. Morales P. Santos-Sanz Absolute magnitudes and phase coefficients of trans-Neptunian objects Astronomy & Astrophysics February 2016 586 A155 33 free 10.1051/0004-6361/201527161 1511.09401 2016A&A...586A.155A 119219851 etal Audrey Thirouin Scott S. Ortiz Keith S. Noll Nicholas A. Moskovitz Jose Luis Ortiz Alain Doressoundiram Rotational Properties of the Haumea Family Members and Candidates: Short-term Variability The Astronomical Journal June 2016 151 6 148 148 free 10.3847/0004-6256/151/6/148 1603.04406 2016AJ....151..148T 118510175 etal T. Hromakina D. Perna I. Belskaya E. Dotto A. Rossi F. Bisi Photometric observations of nine Transneptunian objects and Centaurs https://www.astrofit2.inaf.it/wp-content/uploads/2018/07/Hromakina2018.pdf Monthly Notices of the Royal Astronomical Society February 2018 474 2 2536–2543 free 10.1093/mnras/stx2904 1712.04284 2018MNRAS.474.2536H 119503877 etal E. Vilenius D. Stansberry T. Müller, T. M. Mueller C. Kiss P. Santos-Sanz "TNOs are Cool": A survey of the trans-Neptunian region. XIV. Size/albedo characterization of the Haumea family observed with Herschel and Spitzer Astronomy & Astrophysics October 2018 618 A136 A136 free 10.1051/0004-6361/201732564 1904.06333 2018A&A...618A.136V Benjamin Proudfoot Darin Ragozzine Modeling the Formation of the Family of the Dwarf Planet Haumea The Astronomical Journal June 2019 6 157 230 230 free 10.3847/1538-3881/ab19c4 2019AJ....157..230P 1904.00038 90262136 Dina Prialnik Maria Antoinetta Barucci Leslie Young José L. Ortiz Bruno Sicardy Julio I. B. Camargo Pablo Santos-Sanz Felipe Braga-Ribas The Trans-Neptunian Solar System Chapter 19 - Stellar occultations by Trans-Neptunian objects: From predictions to observations and prospects for the future 2020 413–437 10.1016/B978-0-12-816490-7.00019-9 1905.04335 2020tnss.book..413O 9780128164907 etal E. Fernández-Valenzuela N. Pinilla-Alonso J. Stansberry J. P. Emery W. Perkins C. Van Laerhoven Compositional Study of Trans-Neptunian Objects at λ > 2.2 μm The Planetary Science Journal February 2021 2 1 10 free 10.3847/PSJ/abc34e 2021PSJ.....2...10F 2011.07121 234003733 Alex H. Parker Transneptunian Space and the Post-Pluto Paradigm The Pluto System After New Horizons University of Arizona Press, Tucson S. A. Stern J. M. Moore W. M. Grundy L. A. Young R. P. Binzel 2021 545–568 10.2458/azu_uapress_9780816540945-ch023 2107.02224 2021psnh.book..545P 978-0-8165-4094-5 229245689 Jessica L. Noviello Steven J. Desch Marc Meveu Benjamin C. N. Proudfoot Sarah Sonnett Let It Go: Geophysically Driven Ejection of the Haumea Family Members The Planetary Science Journal September 2022 3 9 225 225 free 10.3847/PSJ/ac8e03 2022PSJ.....3..225N 252620869 Licandro, J. di Fabrizio, L. Pinilla-Alonso, N. de León, J. Oliva, E. Trans-Neptunian object (55636) 2002 TX 300, a fresh icy surface in the outer Solar System 2006 Astronomy and Astrophysics 457 1 329–333 10.1051/0004-6361:20064906 2006A&A...457..329L free Michael E. Brown Kristina M. Barkume Darin Ragozzine Emily L. Schaller A collisional family of icy objects in the Kuiper belt Nature 446 March 2007 7133 294–296 10.1038/nature05619 17361177 2007Natur.446..294B 4430027 https://resolver.caltech.edu/CaltechAUTHORS:20120925-105447086 External links 55636 55636 (55636) 2002 TX 300 55637 Uni Category:Haumea family Category:Classical Kuiper belt objects Category:Discoveries by NEAT Category:Objects observed by stellar occultation 20021015 Category:Former dwarf planet candidates