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The Haumea or Haumean family is the only identified trans-Neptunian collisional family; that is, the only group of trans-Neptunian objects (TNOs) with similar orbital parameters and spectra (nearly pure water-ice) that suggest they originated in the disruptive impact of a progenitor body.^[1] Calculations indicate that it is probably the only trans-Neptunian collisional family.^[2] Members are known as Haumeids.

Members

Brightest Haumea-family members:
Object	(H)	Diameter albedo=0.7	V–R^[3]
Haumea	0.2	1,460 km	0.33
2002 TX₃₀₀	3.4	332 km	0.36
2003 OP₃₂	3.9	276 km	0.39
2005 RR₄₃	4.1	252 km	0.41
2009 YE₇	4.5	200 km
1995 SM₅₅	4.6	191 km	0.39
2005 CB₇₉	4.7	182 km	0.37
1996 TO₆₆	4.8	174 km	0.39

Characteristics

The dwarf planet Haumea is the largest member of the family, and the core of the differentiated progenitor; other identified members are the moons of Haumea and the Kuiper belt objects (55636) 2002 TX300, (24835) 1995 SM55, (19308) 1996 TO66, (120178) 2003 OP32, (145453) 2005 RR43, (86047) 1999 OY3, (416400) 2003 UZ117, (308193) 2005 CB79, (612620) 2003 SQ317^[3] and (386723) 2009 YE7,^[4] all with an ejection velocity from Haumea of less than 150 m/s.^[5] The brightest Haumeids have absolute magnitudes (H) bright enough to suggest a size between 400 and 700 km in diameter, and so possible dwarf planets, if they had the albedos of typical TNOs; however, they are likely to be much smaller as it is thought they are water-icy bodies with high albedos. The dispersion of the proper orbital elements of the members is a few percent or less (5% for semi-major axis, 1.4° for the inclination and 0.08 for the eccentricity).^[6] The diagram illustrates the orbital elements of the members of the family in relation to other TNOs.^{[citation needed]}

The objects' common physical characteristics include neutral colours and deep infrared absorption features (at 1.5 and 2.0 μm) typical of water ice.^[7]^[8]

Member orbits

Haumea collisional family^[9]
Name	Mean anomaly M°	Epoch	Arg.Per ω	Long Ω°	Incl i°	Ecc e	Semi-major axis a (AU)	H	Albedo
136108 Haumea	217.772	2459000.5	238.779	122.163	28.214	0.195	43.182	0.2	0.66
(19308) 1996 TO66	139.355	2459000.5	242.001	355.158	27.381	0.120	43.345	4.8	0.70
(24835) 1995 SM55	334.598	2459000.5	70.848	21.016	27.042	0.101	41.658	4.6	>0.07
(55636) 2002 TX300	77.718	2459000.5	340.338	324.409	25.832	0.126	43.270	3.4	0.88
(86047) 1999 OY3	64.735	2459000.5	306.961	301.717	24.154	0.173	44.158	6.8	0.70
(120178) 2003 OP32	72.355	2459000.5	71.889	182.016	27.135	0.109	43.496	4.0	0.70
(145453) 2005 RR43	50.329	2459000.5	278.004	85.792	28.574	0.139	43.112	4.0	0.703
(202421) 2005 UQ513^{[note 1]}	228.669	2459000.5	222.480	307.532	25.699	0.145	43.329	3.6	0.31
(308193) 2005 CB79	322.348	2459000.5	92.975	112.936	28.692	0.142	43.212	4.6	0.70
(315530) 2008 AP129	53.949	2459000.5	56.289	14.875	27.419	0.136	41.546	4.7
(386723) 2009 YE7	183.830	2459000.5	101.182	141.381	29.114	0.147	44.203	4.3	0.70
(416400) 2003 UZ117	344.334	2459000.5	246.134	204.629	27.429	0.129	44.031	5.1
(523645) 2010 VK201	171.302	2459000.5	89.649	156.308	28.839	0.116	43.091	5.0
(543454) 2014 HZ199	66.295	2459000.5	85.268	57.101	27.835	0.154	43.249	5.0
(612620) 2003 SQ317	11.059	2459000.5	191.080	176.268	28.537	0.082	42.736	6.6	0.05–0.5
(673087) 2015 AJ281	284.578	2459000.5	8.239	256.130	26.805	0.130	43.199	5.0
(671467) 2014 LO28	313.026	2459000.5	104.587	287.074	25.535	0.121	43.219	5.3
(653589) 2014 QW441	1.117	2459000.5	202.336	162.681	28.761	0.106	44.449	5.2

^ 2005 UQ₅₁₃ displays a red spectrum unlike the rest of the Haumea family, although it dynamically belongs in the group.

Resonances with Neptune

The current orbits of the members of the family cannot be accounted for by the formational collision alone. To explain the spread of the orbital elements, an initial velocity dispersion of ≈ 400 m/s is required, but such a velocity spread should have dispersed the fragments much further. This problem applies only to Haumea itself; the orbital elements of all the other objects in the family require an initial velocity dispersion of just ≈ 140 m/s. To explain this mismatch in the required velocity dispersion, Brown and colleagues suggest that Haumea initially had orbital elements closer to those of the other members of the family and its orbit (especially the orbital eccentricity) changed after the collision. Unlike the other members of the family, Haumea is in an intermittent 7:12 resonance with Neptune,^[10] which could have increased Haumea's eccentricity to its current value.^[1]

The Haumea family occupies a region of the Kuiper belt where multiple resonances (including the 3:5, 4:7, 7:12, 10:17 and 11:19 mean motion resonances) interact, leading to the orbital diffusion of that collision family.^[11] Beside the intermittent 7:12 resonance currently occupied by Haumea itself, other members of the family occupy some of the other resonances, and resonance hopping (switching from one resonance to another) is possible on a time scale of hundreds of millions of years. (19308) 1996 TO66, the first member of the Haumea family to be discovered, is currently in an intermittent 11:19 resonance.^[12]

Formation and evolution

Collisional formation of the family requires a progenitor some 1660 km in diameter, with a density of ~2.0 g/cm³, similar to Pluto and Eris. During the formational collision, Haumea lost roughly 20% of its mass, mostly ice, and became denser.^[1]

In addition to the effects of resonances with Neptune, there may be other complications in the origin of the family. It has been suggested that the material ejected in the initial collision may have coalesced into a large moon of Haumea, which gradually increased its distance from Haumea through tidal evolution, and was then later shattered in a second collision, dispersing its shards outwards.^[5] This second scenario produces a velocity dispersion of ~190 m/s, considerably closer to the measured ~140 m/s velocity dispersion of the family members; it also avoids the difficulty of the observed ~140 m/s dispersion being much less than the ~900 m/s escape velocity of Haumea.^[5]

Haumea may not be the only elongated, rapidly rotating, large object in the Kuiper belt. In 2002, Jewitt and Sheppard suggested that Varuna should be elongated, based on its rapid rotation. In the early history of the Solar System, the trans-Neptunian region would have contained many more objects than it does at present, increasing the likelihood of collisions between objects. Gravitational interaction with Neptune has since scattered many objects out of the Kuiper belt to the scattered disc.^{[citation needed]}

The presence of the collisional family hints that Haumea and its "offspring" might have originated in the scattered disc. In today's sparsely populated Kuiper belt, the chance of such a collision occurring over the age of the Solar System is less than 0.1 percent. The family could not have formed in the denser primordial Kuiper belt because such a close-knit group would have been disrupted by Neptune's subsequent migration into the belt, which is thought to have been the cause of its current low density. Therefore, it appears likely that the dynamic scattered disc region, in which the possibility of such a collision is far higher, is the place of origin for the object which would become Haumea and its kin. Simulations suggest the probability of one such family in the Solar System is approximately 50%, so it is possible that the Haumea family is unique.^[2]

Because it would have taken at least a billion years for the group to have diffused as far as it has, the collision that created the Haumea family is thought to have occurred very early in the Solar System's history.^[13] This conflicts with the findings of Rabinowitz and colleagues who found in their studies of the group that their surfaces were remarkably bright; their colour suggests that they have recently (i.e. within the last 100 million years) been resurfaced by fresh ice. Over a timescale as long as a billion years, energy from the Sun would have reddened and darkened their surfaces, and no plausible explanation has been found to account for their apparent youth.^[14]

However, more detailed studies of the visible and near infrared spectrum of Haumea^[15] show it is a homogeneous surface covered by an intimate 1:1 mixture of amorphous and crystalline ice, together with no more than 8% organics. This high amount of amorphous ice on the surface confirms that the collisional event must have happened more than 100 million years ago. This result agrees with the dynamical studies and discards the assumption that the surfaces of these objects are young.^{[citation needed]}

References

^ ^a ^b ^c Brown, Michael E.; Barkume, Kristina M.; Ragozzine, Darin; Schaller, Emily L. (2007). "A collisional family of icy objects in the Kuiper belt" (PDF). Nature. 446 (7133): 294–296. Bibcode:2007Natur.446..294B. doi:10.1038/nature05619. PMID 17361177. S2CID 4430027.
^ ^a ^b Harold F. Levison; Alessandro Morbidelli; David Vokrouhlický; William F. Bottke (2008). "On a Scattered Disc Origin for the 2003 EL₆₁ Collisional Family—an Example of the Importance of Collisions in the Dynamics of Small Bodies". The Astronomical Journal. 136 (3): 1079–1088. arXiv:0809.0553. Bibcode:2008AJ....136.1079L. doi:10.1088/0004-6256/136/3/1079. S2CID 10861444.
^ ^a ^b Snodgrass, Carry, Dumas, Hainaut (16 December 2009). "Characterisation of candidate members of (136108) Haumea's family". Astronomy and Astrophysics. 511: A72. arXiv:0912.3171. Bibcode:2010A&A...511A..72S. doi:10.1051/0004-6361/200913031.{{cite journal}}: CS1 maint: multiple names: authors list (link)
^ Trujillo, Sheppard and Schaller (14 February 2011). "A Photometric System for Detection of Water and Methane Ices on Kuiper Belt Objects". The Astrophysical Journal. 730 (2): 105. arXiv:1102.1971. Bibcode:2011ApJ...730..105T. doi:10.1088/0004-637X/730/2/105. S2CID 53942260.
^ ^a ^b ^c Schlichting, Hilke E.; Re'em Sari (2009). "The Creation of Haumea's Collisional Family". The Astrophysical Journal. 700 (2): 1242–1246. arXiv:0906.3893. Bibcode:2009ApJ...700.1242S. doi:10.1088/0004-637X/700/2/1242. S2CID 19022987.
^ de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (1 February 2018). "Dynamically correlated minor bodies in the outer Solar system". Monthly Notices of the Royal Astronomical Society. 474 (1): 838–846. arXiv:1710.07610. Bibcode:2018MNRAS.474..838D. doi:10.1093/mnras/stx2765.
^ Pinilla-Alonso, N.; Licandro, J.; Gil-Hutton, R.; Brunetto, R. (2007). "The water ice rich surface of (145453) 2005 RR43: A case for a carbon-depleted population of TNOs?". Astronomy and Astrophysics. 468 (1): L25. arXiv:astro-ph/0703098. Bibcode:2007A&A...468L..25P. doi:10.1051/0004-6361:20077294. S2CID 18546361.
^ Pinilla-Alonso, N.; Licandro, J.; Lorenzi, V. (July 2008). "Visible spectroscopy in the neighborhood of 2003EL{61}". Astronomy and Astrophysics. 489 (1): 455–458. arXiv:0807.2670. Bibcode:2008A&A...489..455P. doi:10.1051/0004-6361:200810226. S2CID 56098887.
^ Proudfoot, Benjamin; Ragozzine, Darin (May 2019). "Modeling the Formation of the Family of the Dwarf Planet Haumea". The Astronomical Journal. 157 (6): 230. arXiv:1904.00038. Bibcode:2019AJ....157..230P. doi:10.3847/1538-3881/ab19c4. S2CID 90262136.
^ Mark Buie, Orbit Fit and Astrometric record for 136108, 11 November 2019
^ Ragozzine & Brown, Candidate Members and Age Estimate of the Family of Kuiper Belt Object 2003 EL61, submitted 4 Sep 2007
^ D. Ragozzine; M. E. Brown (2007-09-04). "Candidate Members and Age Estimate of the Family of Kuiper Belt Object 2003 EL₆₁". The Astronomical Journal. 134 (6): 2160–2167. arXiv:0709.0328. Bibcode:2007AJ....134.2160R. doi:10.1086/522334. S2CID 8387493.
^ D. Ragozzine; M. E. Brown (2007). "Candidate Members and Age Estimate of the Family of Kuiper Belt Object 2003 EL₆₁". The Astronomical Journal. 134 (6): 2160–2167. arXiv:0709.0328. Bibcode:2007AJ....134.2160R. doi:10.1086/522334. S2CID 8387493.
^ David L. Rabinowitz; Bradley E. Schaefer; Martha W. Schaefer; Suzanne W. Tourtellotte (2008). "The Youthful Appearance of the 2003 EL61 Collisional Family". The Astronomical Journal. 136 (4): 1502–1509. arXiv:0804.2864. Bibcode:2008AJ....136.1502R. doi:10.1088/0004-6256/136/4/1502. S2CID 117167835.
^ N. Pinilla-Alonso; R. Brunetto; J. Licandro; R. Gil-Hutton; T. L. Roush; G. Strazzulla (March 2009). "Study of the Surface of 2003 EL61, the largest carbon-depleted object in the trans-neptunian belt". Astronomy and Astrophysics. 496 (2): 547. arXiv:0803.1080. Bibcode:2009A&A...496..547P. doi:10.1051/0004-6361/200809733. S2CID 15139257.

External links

http://news.softpedia.com/news/New-Body-Parts-From-Kuiper-Belt-039-s-Haumea-95833.shtml

[10] 2005 UQ₅₁₃ displays a red spectrum unlike the rest of the Haumea family, although it dynamically belongs in the group.

[BrownBarkume2007-1] Brown, Michael E.; Barkume, Kristina M.; Ragozzine, Darin; Schaller, Emily L. (2007). "A collisional family of icy objects in the Kuiper belt" (PDF). Nature. 446 (7133): 294–296. Bibcode:2007Natur.446..294B. doi:10.1038/nature05619. PMID 17361177. S2CID 4430027.

[Levison-2] Harold F. Levison; Alessandro Morbidelli; David Vokrouhlický; William F. Bottke (2008). "On a Scattered Disc Origin for the 2003 EL₆₁ Collisional Family—an Example of the Importance of Collisions in the Dynamics of Small Bodies". The Astronomical Journal. 136 (3): 1079–1088. arXiv:0809.0553. Bibcode:2008AJ....136.1079L. doi:10.1088/0004-6256/136/3/1079. S2CID 10861444.

[Snodgrass2009-3] Snodgrass, Carry, Dumas, Hainaut (16 December 2009). "Characterisation of candidate members of (136108) Haumea's family". Astronomy and Astrophysics. 511: A72. arXiv:0912.3171. Bibcode:2010A&A...511A..72S. doi:10.1051/0004-6361/200913031.{{cite journal}}: CS1 maint: multiple names: authors list (link)

[Trujillo2011-4] Trujillo, Sheppard and Schaller (14 February 2011). "A Photometric System for Detection of Water and Methane Ices on Kuiper Belt Objects". The Astrophysical Journal. 730 (2): 105. arXiv:1102.1971. Bibcode:2011ApJ...730..105T. doi:10.1088/0004-637X/730/2/105. S2CID 53942260.

[SchlichtingSari2009-5] Schlichting, Hilke E.; Re'em Sari (2009). "The Creation of Haumea's Collisional Family". The Astrophysical Journal. 700 (2): 1242–1246. arXiv:0906.3893. Bibcode:2009ApJ...700.1242S. doi:10.1088/0004-637X/700/2/1242. S2CID 19022987.

[pairs-6] Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (1 February 2018). "Dynamically correlated minor bodies in the outer Solar system". Monthly Notices of the Royal Astronomical Society. 474 (1): 838–846. arXiv:1710.07610. Bibcode:2018MNRAS.474..838D. doi:10.1093/mnras/stx2765.

[Pinilla-Alonso2007-7] Pinilla-Alonso, N.; Licandro, J.; Gil-Hutton, R.; Brunetto, R. (2007). "The water ice rich surface of (145453) 2005 RR43: A case for a carbon-depleted population of TNOs?". Astronomy and Astrophysics. 468 (1): L25. arXiv:astro-ph/0703098. Bibcode:2007A&A...468L..25P. doi:10.1051/0004-6361:20077294. S2CID 18546361.

[8] Pinilla-Alonso, N.; Licandro, J.; Lorenzi, V. (July 2008). "Visible spectroscopy in the neighborhood of 2003EL{61}". Astronomy and Astrophysics. 489 (1): 455–458. arXiv:0807.2670. Bibcode:2008A&A...489..455P. doi:10.1051/0004-6361:200810226. S2CID 56098887.

[Proudfoot2019-9] Proudfoot, Benjamin; Ragozzine, Darin (May 2019). "Modeling the Formation of the Family of the Dwarf Planet Haumea". The Astronomical Journal. 157 (6): 230. arXiv:1904.00038. Bibcode:2019AJ....157..230P. doi:10.3847/1538-3881/ab19c4. S2CID 90262136.

[11] Mark Buie, Orbit Fit and Astrometric record for 136108, 11 November 2019

[12] Ragozzine & Brown, Candidate Members and Age Estimate of the Family of Kuiper Belt Object 2003 EL61, submitted 4 Sep 2007

[resonance-13] D. Ragozzine; M. E. Brown (2007-09-04). "Candidate Members and Age Estimate of the Family of Kuiper Belt Object 2003 EL₆₁". The Astronomical Journal. 134 (6): 2160–2167. arXiv:0709.0328. Bibcode:2007AJ....134.2160R. doi:10.1086/522334. S2CID 8387493.

[14] D. Ragozzine; M. E. Brown (2007). "Candidate Members and Age Estimate of the Family of Kuiper Belt Object 2003 EL₆₁". The Astronomical Journal. 134 (6): 2160–2167. arXiv:0709.0328. Bibcode:2007AJ....134.2160R. doi:10.1086/522334. S2CID 8387493.

[15] David L. Rabinowitz; Bradley E. Schaefer; Martha W. Schaefer; Suzanne W. Tourtellotte (2008). "The Youthful Appearance of the 2003 EL61 Collisional Family". The Astronomical Journal. 136 (4): 1502–1509. arXiv:0804.2864. Bibcode:2008AJ....136.1502R. doi:10.1088/0004-6256/136/4/1502. S2CID 117167835.

[16] N. Pinilla-Alonso; R. Brunetto; J. Licandro; R. Gil-Hutton; T. L. Roush; G. Strazzulla (March 2009). "Study of the Surface of 2003 EL61, the largest carbon-depleted object in the trans-neptunian belt". Astronomy and Astrophysics. 496 (2): 547. arXiv:0803.1080. Bibcode:2009A&A...496..547P. doi:10.1051/0004-6361/200809733. S2CID 15139257.

[1]

[2]

[3]

[4]

[5]

[6]

[7]

[8]

[9]

[note 1]

[10]

[11]

[12]

[13]

[14]

[15]

@@ Line 1: / Line 1: @@
+{{for|the film character Haumeid|She (1965 film)}}
-[[Image:TheKuiperBelt 60AU ELgroup.svg|right|thumb|300px|The collisional family of Haumea (in green), other [[cubewano|classical KBO]] (blue), [[Plutino]]s and other  [[Resonant Trans-Neptunian Object|resonant object]]s (red) and [[scattered disk|SDO]] (grey).  Radius is semi-major axis, angle orbital inclination.]]
+[[Image:TheKuiperBelt 60AU ELgroup.svg|right|thumb|300px|The collisional family of Haumea (in green), other [[cubewano|classical KBO]] (blue), [[Plutino]]s and other [[Resonant Trans-Neptunian Object|resonant object]]s (red) and [[scattered disk|SDO]] (grey).  Radius is semi-major axis, angle orbital inclination.]]
-The '''Haumea''' or '''Haumean family''' is the only identified [[Trans-Neptunian objects|trans-Neptunian]] [[collisional family]]; that is, the only group of trans-Neptunian objects (TNOs) with similar orbital parameters and spectra (nearly pure water-ice) that suggest they originated in the disruptive impact of a progenitor body.<ref name="BrownBarkume2007">{{cite journal |last=Brown |first=Michael E. |author2=Barkume, Kristina M. |author3=Ragozzine, Darin |author4= Schaller, Emily L.  |date=2007 |title=A collisional family of icy objects in the Kuiper belt |journal=Nature |volume=446 |issue=7133 |pages=294–296 |doi=10.1038/nature05619 |pmid=17361177 |bibcode = 2007Natur.446..294B }}</ref> Calculations indicate that it is probably the only trans-Neptunian collisional family.<ref name=Levison/>
+The '''Haumea''' or '''Haumean family''' is the only identified [[Trans-Neptunian objects|trans-Neptunian]] [[collisional family]]; that is, the only group of trans-Neptunian objects (TNOs) with similar orbital parameters and spectra (nearly pure water-ice) that suggest they originated in the disruptive impact of a progenitor body.<ref name="BrownBarkume2007">{{cite journal |last=Brown |first=Michael E. |author2=Barkume, Kristina M. |author3=Ragozzine, Darin |author4= Schaller, Emily L.  |date=2007 |title=A collisional family of icy objects in the Kuiper belt |journal=Nature |volume=446 |issue=7133 |pages=294–296 |doi=10.1038/nature05619 |pmid=17361177 |bibcode = 2007Natur.446..294B |s2cid=4430027 |url=https://authors.library.caltech.edu/34346/2/nature05619-s1.pdf }}</ref> Calculations indicate that it is probably the only trans-Neptunian collisional family.<ref name=Levison/>
+Members are known as '''Haumeids'''.
+==Members==
-<div style="float:right; margin:2px;">
 {| class=wikitable style="text-align:center"
 |+ Brightest Haumea-family members:
 !Object!![[Absolute magnitude#Solar System bodies (H)|(H)]]!!Diameter<br>[[Albedo#Astronomical albedo|albedo]]=0.7!![[Trans-Neptunian object#Colors|V–R]]<ref name="Snodgrass2009">{{Cite journal |author=Snodgrass, Carry, Dumas, Hainaut |title=Characterisation of candidate members of (136108) Haumea's family |journal=Astronomy and Astrophysics|date=16 December 2009|arxiv=0912.3171|doi = 10.1051/0004-6361/200913031 |volume=511 |pages=A72 |bibcode=2010A&A...511A..72S}}</ref>
 |-
-|[[Haumea (dwarf planet)|Haumea]]||0.2||1,632&nbsp;km||0.33
+|[[Haumea (dwarf planet)|Haumea]]||0.2||1,460&nbsp;km||0.33
 |-
 |[[(55636) 2002 TX300|2002 TX<sub>300</sub>]]||3.4||332&nbsp;km||0.36
@@ Line 23: / Line 25: @@
 |-
 |[[(19308) 1996 TO66|1996 TO<sub>66</sub>]]||4.8||174&nbsp;km||0.39
-|}</div>
+|}
-[[File:Haumea family orbits.png|300px|thumb|Orbits of Haumea family members, sharing [[semimajor axes]] around 43 AU, and inclinations around 27°.]]
 ==Characteristics==
+[[File:Haumea family orbits.png|300px|thumb|Orbits of Haumea family members, sharing [[semimajor axes]] around 43 AU, and inclinations around 27°.]]
-The [[dwarf planet]] {{dp|Haumea}} is the largest member of the family, and the core of the differentiated progenitor; other identified members are the [[moons of Haumea]] and the [[Kuiper belt object]]s {{mpl|(55636) 2002 TX|300}}, {{mpl|(24835) 1995 SM|55}}, {{mpl|(19308) 1996 TO|66}},  {{mpl|(120178) 2003 OP|32}}, {{mpl|(145453) 2005 RR|43}}, {{mpl|(86047) 1999 OY|3}}, {{mpl|(416400) 2003 UZ|117}}, {{mpl|(308193) 2005 CB|79}}, {{mpl|2003 SQ|317}}<ref name="Snodgrass2009"/> and {{mpl|(386723) 2009 YE|7}},<ref name="Trujillo2011">{{Cite journal |author=Trujillo, Sheppard and Schaller |title=A Photometric System for Detection of Water and Methane Ices on Kuiper Belt Objects |journal=The [[Astrophysical Journal]] |date=14 February 2011|arxiv=1102.1971|bibcode = 2011ApJ...730..105T |doi = 10.1088/0004-637X/730/2/105 |volume=730 |issue=2 |pages=105 }}</ref> all with an ejection velocity from Haumea of less than 150&nbsp;m/s.<ref name="SchlichtingSari2009"/> The brightest Haumeids have [[Absolute magnitude#Solar System bodies (H)|absolute magnitudes (H)]] bright enough to suggest a size between 400 and 700&nbsp;km in diameter, and so [[List of possible dwarf planets|possible dwarf planets]], if they had the [[Albedo#Astronomical albedo|albedos]] of typical TNOs; however, they are likely to be much smaller as it is thought they are water-icy bodies with high albedos. The dispersion of the [[proper orbital elements]] of the members is a few percent or less (5% for [[semi-major axis]], 1.4°  for the [[orbital inclination|inclination]] and 0.08 for the [[orbital eccentricity|eccentricity]]).<ref name=pairs>{{cite journal
+The [[dwarf planet]] {{dp|Haumea}} is the largest member of the family, and the core of the differentiated progenitor; other identified members are the [[moons of Haumea]] and the [[Kuiper belt object]]s {{mpl|(55636) 2002 TX|300}}, {{mpl|(24835) 1995 SM|55}}, {{mpl|(19308) 1996 TO|66}},  {{mpl|(120178) 2003 OP|32}}, {{mpl|(145453) 2005 RR|43}}, {{mpl|(86047) 1999 OY|3}}, {{mpl|(416400) 2003 UZ|117}}, {{mpl|(308193) 2005 CB|79}}, {{mpl|(612620) 2003 SQ|317}}<ref name="Snodgrass2009"/> and {{mpl|(386723) 2009 YE|7}},<ref name="Trujillo2011">{{Cite journal |author=Trujillo, Sheppard and Schaller |title=A Photometric System for Detection of Water and Methane Ices on Kuiper Belt Objects |journal=The Astrophysical Journal |date=14 February 2011|arxiv=1102.1971|bibcode = 2011ApJ...730..105T |doi = 10.1088/0004-637X/730/2/105 |volume=730 |issue=2 |pages=105 |s2cid=53942260 }}</ref> all with an ejection velocity from Haumea of less than 150&nbsp;m/s.<ref name="SchlichtingSari2009"/> The brightest Haumeids have [[Absolute magnitude#Solar System bodies (H)|absolute magnitudes (H)]] bright enough to suggest a size between 400 and 700&nbsp;km in diameter, and so [[List of possible dwarf planets|possible dwarf planets]], if they had the [[Albedo#Astronomical albedo|albedos]] of typical TNOs; however, they are likely to be much smaller as it is thought they are water-icy bodies with high albedos. The dispersion of the [[proper orbital elements]] of the members is a few percent or less (5% for [[semi-major axis]], 1.4°  for the [[orbital inclination|inclination]] and 0.08 for the [[orbital eccentricity|eccentricity]]).<ref name=pairs>{{cite journal
   |last1=de la Fuente Marcos |first1=Carlos
   |last2=de la Fuente Marcos |first2=Raúl
@@ Line 33: / Line 35: @@
   |journal=[[Monthly Notices of the Royal Astronomical Society]]
   |date=1 February 2018
-  |volume= |issue=
+  |volume= 474|issue=1
   |arxiv=1710.07610
   |doi=10.1093/mnras/stx2765
-  |pages=
+  |pages=838–846
+  |doi-access=free
-  |url=http://adsabs.harvard.edu/abs/2017arXiv171007610D
-  |bibcode = 2017arXiv171007610D }}</ref> The diagram illustrates the orbital elements of the members of the family in relation to other [[Trans-Neptunian object|TNO]]s.{{citation needed|date=January 2011}}
+ |bibcode = 2018MNRAS.474..838D }}</ref> The diagram illustrates the orbital elements of the members of the family in relation to other [[Trans-Neptunian object|TNO]]s.{{citation needed|date=January 2011}}
 The objects' common physical characteristics include neutral [[color index|colours]] and deep infrared absorption features (at 1.5 and 2.0 [[micrometres|μm]]) typical of water ice.<ref name="Pinilla-Alonso2007">
 {{cite journal
  |doi=10.1051/0004-6361:20077294
- |title=The water ice rich surface of (145453) 2005 RR43:    A case for a   carbon-depleted population of TNOs?
+ |title=The water ice rich surface of (145453) 2005 RR43: A case for a carbon-depleted population of TNOs?
  |date=2007
  |last1=Pinilla-Alonso
@@ Line 55: / Line 57: @@
  |journal=Astronomy and Astrophysics
  |volume=468
+ |issue=1
  |pages=L25
-|arxiv = astro-ph/0703098 |bibcode = 2007A&A...468L..25P }}</ref><ref>
+|arxiv = astro-ph/0703098 |bibcode = 2007A&A...468L..25P |s2cid=18546361
+ }}</ref><ref>
   {{cite journal
   | title = Visible spectroscopy in the neighborhood of 2003EL{61}
   |author1=Pinilla-Alonso, N. |author2=Licandro, J. |author3=Lorenzi, V. | journal = Astronomy and Astrophysics
   | date = July 2008| volume =489 | issue = 1
-  | bibcode=2008A&A...489..455P |doi = 10.1051/0004-6361:200810226 |arxiv = 0807.2670 }}
+  |pages=455–458 | bibcode=2008A&A...489..455P |doi = 10.1051/0004-6361:200810226 |arxiv = 0807.2670 |s2cid=56098887 }}
 </ref>
-=== Member orbits===
+=== Member orbits ===
 <!-- To complete...
 {| class="wikitable"
@@ Line 84: / Line 88: @@
 {| class="wikitable sortable"
+|+ Haumea collisional family<ref name="Proudfoot2019">{{cite journal|title=Modeling the Formation of the Family of the Dwarf Planet Haumea|first1=Benjamin|last1=Proudfoot|first2=Darin|last2=Ragozzine|journal=The Astronomical Journal|date=May 2019|volume=157 |issue=6 |page=230 |arxiv=1904.00038|doi=10.3847/1538-3881/ab19c4|bibcode=2019AJ....157..230P |s2cid=90262136 |doi-access=free }}</ref>
-|+ Haumea collisional family
 !Name||[[Mean anomaly]]<BR>M°||Epoch||[[Argument of perihelion|Arg.Per]]<BR>ω||[[Longitude of the ascending node|Long]]<BR>Ω°||[[Orbital inclination|Incl]]<BR>i°||[[Orbital eccentricity|Ecc]]<BR>e||[[Semi-major axis]]<br>a (AU)||[[Absolute magnitude|H]]||[[Albedo]]
 |-
-|[[136108 Haumea]]||214.0634158||2458000.5||238.8703238||121.9703096||28.20363528||0.189364867||43.35540773||0.2||0.51
+|[[136108 Haumea]]||217.772||2459000.5||238.779||122.163||28.214||0.195||43.182||0.2||{{sort|0.660|0.66}}
 |-
-|{{mpl|(19308) 1996 TO|66}}||138.3198033||2458000.5||239.7392156||355.2685304||27.47641085||0.12266934||43.14574924||4.8||0.7
+|{{mpl|(19308) 1996 TO|66}}||139.355||2459000.5||242.001||355.158||27.381||0.120||43.345||4.8||{{sort|0.700|0.70}}
 |-
-|{{mpl|(24835) 1995 SM|55}}||329.4502628||2458000.5||72.59972842||21.10934028||27.09627096||0.101904744||41.62783812||4.6||0.7
+|{{mpl|(24835) 1995 SM|55}}||334.598||2459000.5||70.848||21.016||27.042||0.101||41.658||4.6||{{sort|0.070|>0.07}}
 |-
-|{{mpl|(55636) 2002 TX|300}}||76.40323137||2458000.5||338.2748696||324.6074846||25.86217729||0.123449237||43.06538353||3.4||0.88
+|{{mpl|(55636) 2002 TX|300}}||77.718||2459000.5||340.338||324.409||25.832||0.126||43.270||3.4||{{sort|0.880|0.88}}
 |-
-|{{mpl|(86047) 1999 OY|3}}||63.50398705||2458000.5||304.6112431||301.7996763||24.21502662||0.172640468||43.85255215||6.8||0.7
+|{{mpl|(86047) 1999 OY|3}}||64.735||2459000.5||306.961||301.717||24.154||0.173||44.158||6.8||{{sort|0.700|0.70}}
 |-
-|{{mpl|(120178) 2003 OP|32}}||72.4411346||2458000.5||68.38278265||182.9360269||27.21328678||0.108234874||43.18272472||3.9||0.7
+|{{mpl|(120178) 2003 OP|32}}||72.355||2459000.5||71.889||182.016||27.135||0.109||43.496||4.0||{{sort|0.700|0.70}}
 |-
-|{{mpl|(145453) 2005 RR|43}}||46.80125338||2458000.5||278.4115508||85.81006564||28.55289669||0.135779523||43.039267||4.1||0.70
+|{{mpl|(145453) 2005 RR|43}}||50.329||2459000.5||278.004||85.792||28.574||0.139||43.112||4.0||{{sort|0.703|0.703}}
 |-
+|{{mpl|(202421) 2005 UQ|513}}<ref group="note">{{mp|2005 UQ|513}} displays a red spectrum unlike the rest of the Haumea family, although it dynamically belongs in the group.</ref>
-|{{mpl|(308193) 2005 CB|79}}||320.8370758||2458000.5||91.1455215||112.8524839||28.64647725||0.146744922||43.55516216||4.7||0.70
+||228.669||2459000.5||222.480||307.532||25.699||0.145||43.329||3.6||{{sort|0.310|0.31}}
 |-
-|{{mpl|(386723) 2009 YE|7}}||182.1347546||2458000.5||99.74202013||141.6075597||29.08966805||0.147800174||44.16498071||4.5||0.70
+|{{mpl|(308193) 2005 CB|79}}||322.348||2459000.5||92.975||112.936||28.692||0.142||43.212||4.6||{{sort|0.700|0.70}}
 |-
-|{{mpl|(416400) 2003 UZ|117}}||339.9307571||2458000.5||247.448259||204.721906||27.47252328||0.129983806||44.05112933||5.3||
+|{{mpl|(315530) 2008 AP|129}}||53.949||2459000.5||56.289||14.875||27.419||0.136||41.546||4.7||
 |-
-|{{mpl|2003 SQ|317}}||6.946737862||2458000.5||191.8082104||176.337805||28.61851436||0.076663828||42.48850031||6.2||0.05-0.5
+|{{mpl|(386723) 2009 YE|7}}||183.830||2459000.5||101.182||141.381||29.114||0.147||44.203||4.3||{{sort|0.700|0.70}}
+|-
+|{{mpl|(416400) 2003 UZ|117}}||344.334||2459000.5||246.134||204.629||27.429||0.129||44.031||5.1||
+|-
+|{{mpl|(523645) 2010 VK|201}}||171.302||2459000.5||89.649||156.308||28.839||0.116||43.091||5.0||
+|-
+|{{mpl|(543454) 2014 HZ|199}}||66.295||2459000.5||85.268||57.101||27.835||0.154||43.249||5.0||
+|-
+|{{mpl|(612620) 2003 SQ|317}}||11.059||2459000.5||191.080||176.268||28.537||0.082||42.736||6.6||{{sort|0.050|0.05–0.5}}
+|-
+|{{mpl|(673087) 2015 AJ|281}} ||284.578||2459000.5||8.239||256.130||26.805||0.130||43.199||5.0||
+|-
+|{{mpl|(671467) 2014 LO|28}}||313.026||2459000.5||104.587||287.074||25.535||0.121||43.219||5.3||
+|-
+|{{mpl|(653589) 2014 QW|441}}||1.117||2459000.5||202.336||162.681||28.761||0.106||44.449||5.2||
 |}
+{{Reflist|group="note"}}
+===Resonances with Neptune===
+The current orbits of the members of the family cannot be accounted for by the formational collision alone. To explain the spread of the orbital elements, an initial velocity dispersion of ≈&nbsp;400 [[Metre per second|m/s]] is required, but such a velocity spread should have dispersed the fragments much further. This problem applies only to Haumea itself; the orbital elements of all the other objects in the family require an initial velocity dispersion of just ≈&nbsp;140&nbsp;m/s. To explain this mismatch in the required velocity dispersion, Brown and colleagues suggest that Haumea initially had orbital elements closer to those of the other members of the family and its orbit (especially the orbital eccentricity) changed after the collision. Unlike the other members of the family, Haumea is in an intermittent 7:12 [[orbital resonance|resonance]] with Neptune,<ref>Mark Buie, [https://www.boulder.swri.edu/~buie/kbo/astrom/136108.html Orbit Fit and Astrometric record for 136108], 11 November 2019</ref> which could have increased Haumea's eccentricity to its current value.<ref name="BrownBarkume2007"/>
+The Haumea family occupies a region of the Kuiper belt where multiple resonances (including the [[Resonant trans-Neptunian object|3:5, 4:7, 7:12, 10:17 and 11:19 mean motion resonances]]) interact, leading to the orbital diffusion of that collision family.<ref>Ragozzine & Brown, [https://arxiv.org/abs/0709.0328 Candidate Members and Age Estimate of the Family of Kuiper Belt Object 2003 EL61], submitted 4 Sep 2007</ref> Beside the intermittent 7:12 resonance currently occupied by Haumea itself, other members of the family occupy some of the other resonances, and resonance hopping (switching from one resonance to another) is possible on a time scale of hundreds of millions of years. {{mpl|(19308) 1996 TO|66}}, the first member of the Haumea family to be discovered, is currently in an intermittent 11:19 resonance.<ref name="resonance">{{cite journal
+  |title=Candidate Members and Age Estimate of the Family of Kuiper Belt Object {{mp|2003 EL|61}}
+  |author=D. Ragozzine
+  |author2=M. E. Brown
+  |journal=The Astronomical Journal
+  |volume=134 |issue=6 |pages= 2160–2167
+  |date=2007-09-04
+  |bibcode=2007AJ....134.2160R
+  |doi=10.1086/522334
+  |arxiv=0709.0328|s2cid=8387493
+ }}</ref>
 ==Formation and evolution==
 Collisional formation of the family requires a progenitor some 1660&nbsp;km in diameter, with a density of ~2.0 g/cm<sup>3</sup>, similar to [[Pluto]] and [[Eris (dwarf planet)|Eris]]. During the formational collision, Haumea lost roughly 20% of its mass, mostly ice, and became denser.<ref name="BrownBarkume2007"/>
+In addition to the effects of resonances with Neptune, there may be other complications in the origin of the family. It has been suggested that the material ejected in the initial collision may have coalesced into a large moon of Haumea, which gradually increased its distance from Haumea through [[Tidal acceleration|tidal evolution]], and was then later shattered in a second collision, dispersing its shards outwards.<ref name="SchlichtingSari2009"/> This second scenario produces a velocity dispersion of ~190&nbsp;m/s, considerably closer to the measured ~140&nbsp;m/s velocity dispersion of the family members; it also avoids the difficulty of the observed ~140&nbsp;m/s dispersion being much less than the ~900&nbsp;m/s escape velocity of Haumea.<ref name="SchlichtingSari2009">
-The current orbits of the members of the family cannot be accounted for by the formational collision alone. To explain the spread of the orbital elements, an initial velocity dispersion of ~400 [[Metre per second|m/s]] is required, but such a velocity spread should have dispersed the fragments much further. This problem applies only to Haumea itself; the orbital elements of all the other objects in the family require an initial velocity dispersion of ~140&nbsp;m/s. To explain this mismatch in the required velocity dispersion, Brown and colleagues suggest that Haumea initially had orbital elements closer to those of the other members of the family and its orbit (especially the orbital eccentricity), changed ''after'' the collision. Unlike the other members of the family, Haumea is in a chaotic orbit, near the 7:12 [[orbital resonance|resonance]] with Neptune, which would increase Haumea's eccentricity to its current value.<ref name="BrownBarkume2007"/>
-A second proposal suggests a more complicated origin for the family: that the material ejected in the initial collision instead coalesced into a large moon of Haumea, which gradually increased its distance from Haumea through [[Tidal acceleration|tidal evolution]], and was then later shattered in a second collision, dispersing its shards outwards.<ref name="SchlichtingSari2009"/> This second scenario produces a velocity dispersion of ~190&nbsp;m/s, considerably closer to the measured ~140&nbsp;m/s velocity dispersion of the family members; it also avoids the difficulty of the observed ~140&nbsp;m/s dispersion being much less than the ~900&nbsp;m/s escape velocity of Haumea.<ref name="SchlichtingSari2009">
   {{cite journal
   |last=Schlichting
@@ Line 126: / Line 159: @@
   |volume=700
   |issue=2
-  |pages=1242–1246 }}
+  |pages=1242–1246 |s2cid=19022987
+ }}
 </ref>
 Haumea may not be the only elongated, rapidly rotating, large object in the [[Kuiper belt]].  In 2002, Jewitt and Sheppard [[20000 Varuna#References|suggested]] that {{dp|Varuna}} should be elongated, based on its rapid rotation. In the early history of the [[Solar System]], the trans-Neptunian region would have contained many more objects than it does at present, increasing the likelihood of collisions between objects. Gravitational interaction with [[Neptune]] has since scattered many objects out of the Kuiper belt to the [[scattered disc]].{{citation needed|date=January 2011}}
-The presence of the collisional family hints that Haumea and its "offspring" might have originated in the [[scattered disc]]. In today's sparsely populated Kuiper belt, the chance of such a collision occurring over the age of the Solar System is less than 0.1 percent. The family could not have formed in the denser primordial Kuiper belt because such a close-knit group would have been disrupted by [[Neptune#Formation and migration|Neptune's subsequent migration]] into the belt, which is thought to have been the cause of its current low density. Therefore, it appears likely that the dynamic scattered disc region, in which the possibility of such a collision is far higher, is the place of origin for the object which would become Haumea and its kin. Simulations suggest the probability of one such family in the Solar System is approximately 50%, so it is possible that the Haumea family is unique.<ref name=Levison>{{cite journal|title=On a Scattered Disc Origin for the {{mp|2003 EL|61}} Collisional Family—an  Example of the Importance of Collisions in the Dynamics of Small Bodies|author1=Harold F. Levison |author2=Alessandro Morbidelli |author3=David Vokrouhlický |author4=William F. Bottke |date=2008|journal= The Astronomical Journal|volume= 136|pages= 1079–1088| doi= 10.1088/0004-6256/136/3/1079 |bibcode=2008AJ....136.1079L|issue=3|arxiv = 0809.0553 }}</ref>
+The presence of the collisional family hints that Haumea and its "offspring" might have originated in the [[scattered disc]]. In today's sparsely populated Kuiper belt, the chance of such a collision occurring over the age of the Solar System is less than 0.1 percent. The family could not have formed in the denser primordial Kuiper belt because such a close-knit group would have been disrupted by [[Neptune#Formation and migration|Neptune's subsequent migration]] into the belt, which is thought to have been the cause of its current low density. Therefore, it appears likely that the dynamic scattered disc region, in which the possibility of such a collision is far higher, is the place of origin for the object which would become Haumea and its kin. Simulations suggest the probability of one such family in the Solar System is approximately 50%, so it is possible that the Haumea family is unique.<ref name=Levison>{{cite journal|title=On a Scattered Disc Origin for the {{mp|2003 EL|61}} Collisional Family—an Example of the Importance of Collisions in the Dynamics of Small Bodies|author1=Harold F. Levison |author2=Alessandro Morbidelli |author3=David Vokrouhlický |author4=William F. Bottke |date=2008|journal= The Astronomical Journal|volume= 136|pages= 1079–1088| doi= 10.1088/0004-6256/136/3/1079 |bibcode=2008AJ....136.1079L|issue=3|arxiv = 0809.0553 |s2cid=10861444 }}</ref>
 [[File:TheTransneptunians Color Distribution-2005RR43.png|right|thumb|400px|The + marks {{mpl-|145453|2005 RR|43}} (B−V=0.77, V−R=0.41) on this color plot of TNOs. All the other Haumea-family members are located to the lower left of this point.]]
-Because it would have taken at least a billion years for the group to have diffused as far as it has, the collision that created the Haumea family is thought to have occurred very early in the Solar System's history.<ref>{{cite journal | title=Candidate Members and Age Estimate of the Family of Kuiper Belt Object {{mp|2003 EL|61}} |author1=D. Ragozzine |author2=M. E. Brown | journal=The Astronomical Journal | volume=134 | issue=6 | pages=2160–2167 | date=2007 | doi=10.1086/522334 | bibcode=2007AJ....134.2160R | arxiv=0709.0328}}</ref> This conflicts with the findings of Rabinowitz and colleagues who found in their studies of the group that their surfaces were remarkably bright; their colour suggests that they have recently (i.e. within the last 100 million years) been resurfaced by fresh ice. Over a timescale as long as a billion years, energy from the Sun would have reddened and darkened their surfaces, and no plausible explanation has been found to account for their apparent youth.<ref>{{cite journal|title=The Youthful Appearance of the 2003 EL61 Collisional Family|author1=David L. Rabinowitz |author2=Bradley E. Schaefer |author3=Martha W. Schaefer |author4=Suzanne W. Tourtellotte |date=2008 |arxiv=0804.2864|bibcode = 2008AJ....136.1502R |doi = 10.1088/0004-6256/136/4/1502|volume=136|issue=4|pages=1502–1509|journal=The Astronomical Journal }}</ref>
+Because it would have taken at least a billion years for the group to have diffused as far as it has, the collision that created the Haumea family is thought to have occurred very early in the Solar System's history.<ref>{{cite journal | title=Candidate Members and Age Estimate of the Family of Kuiper Belt Object {{mp|2003 EL|61}} |author1=D. Ragozzine |author2=M. E. Brown | journal=The Astronomical Journal | volume=134 | issue=6 | pages=2160–2167 | date=2007 | doi=10.1086/522334 | bibcode=2007AJ....134.2160R | arxiv=0709.0328|s2cid=8387493 }}</ref> This conflicts with the findings of Rabinowitz and colleagues who found in their studies of the group that their surfaces were remarkably bright; their colour suggests that they have recently (i.e. within the last 100 million years) been resurfaced by fresh ice. Over a timescale as long as a billion years, energy from the Sun would have reddened and darkened their surfaces, and no plausible explanation has been found to account for their apparent youth.<ref>{{cite journal|title=The Youthful Appearance of the 2003 EL61 Collisional Family|author1=David L. Rabinowitz |author2=Bradley E. Schaefer |author3=Martha W. Schaefer |author4=Suzanne W. Tourtellotte |date=2008 |arxiv=0804.2864|bibcode = 2008AJ....136.1502R |doi = 10.1088/0004-6256/136/4/1502|volume=136|issue=4|pages=1502–1509|journal=The Astronomical Journal |s2cid=117167835 }}</ref>
 However, more detailed studies of the visible and near infrared spectrum of Haumea<ref>
@@ Line 143: / Line 177: @@
   | bibcode=2009A&A...496..547P
   | doi = 10.1051/0004-6361/200809733
-  | pages = 547|arxiv = 0803.1080 }}
+  | pages = 547|arxiv = 0803.1080 |s2cid=15139257 }}
 </ref> show it is a homogeneous surface covered by an intimate 1:1 mixture of amorphous and crystalline ice, together with no more than 8% organics. This high amount of amorphous ice on the surface confirms that the collisional event must have happened more than 100 million years ago. This result agrees with the dynamical studies and discards the assumption that the surfaces of these objects are young.{{citation needed|date=January 2011}}
@@ Line 161: / Line 195: @@
 {{DEFAULTSORT:Haumea Family}}
-[[Category:Distant minor planet groups and families]]
 [[Category:Haumea family| ]]
+[[Category:Distant minor planet groups and families]]