List of possible dwarf planets

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Illustration of the relative sizes, albedos, and colours of the largest trans-Neptunian objects

It is estimated that there may be 200 dwarf planets in the Kuiper belt of the outer Solar System, and up to 10,000 in the region beyond.^[1]^[2] The International Astronomical Union has accepted four of these: Pluto, Eris, Haumea, and Makemake, as well as Ceres in the inner Solar System. This article lists these and the more likely of the remaining known possibilities.

IAU naming procedures

Limiting values

Colours of trans-Neptunians. Mars and Triton are not to scale. Phoebe and Pholus are not TNOs.

The qualifying feature of dwarf planets is that they "have sufficient mass for their self-gravity to overcome rigid body forces so that they assume a hydrostatic equilibrium (near-spherical shape)."^[4]^[5]^[6] Except for Pluto and Ceres, current observations are insufficient for a direct determination if a body meets this definition. However, Michael Brown estimates that an icy body relaxes into hydrostatic equilibrium at a diameter somewhere between 200 and 400 km.^[1] Thus, all the trans-Neptunian objects (TNOs) listed below are estimated to be at least 400 km in diameter, though not all bodies estimated to be that size are included. The lists are further complicated by bodies such as 1999 TC₃₆ that were at first assumed to be large single objects but were later discovered to be smaller binary or triple systems.^[7]

Ceres is the only identified dwarf planet in the asteroid belt. The most likely other possibility is 4 Vesta, the second-most-massive asteroid; Vesta appears to have a fully differentiated interior and was therefore in equilibrium at some point in its history, though it apparently is not today.^[8] The third-most massive object, 2 Pallas, has a somewhat irregular surface, and is thought to have only a partially differentiated interior. Brown estimates that, since rocky objects are more rigid than icy objects, rocky objects below 900 km in diameter may not be in hydrostatic equilibrium and thus not dwarf planets.^[1]

List by absolute magnitude (H)

Because size estimates are often crude and vary widely, it is less arbitrary to list objects by absolute magnitudes than by diameter. Theoretical minimum diameters correspond to a maximum albedo of 1. Eris has a high albedo of 0.8–0.9, and members of the Haumea family are also thought to be bright, and thus close to the theoretical minimum. However, many objects are thought to be dark due to tholins causing a red-sloped reflectance spectrum, and therefore red objects may be substantially larger than the lower limit.

As of December 2013 there are 168 trans-Neptunian objects, one centaur and 13 asteroids with an absolute magnitude (H) brighter than 6.^[9]

The lists below only show the bodies with magnitudes of H<5 (63 trans-Neptunian object and 3 asteroids) as for H=5 the minimum diameter is only a third of the 400 km limit. For bodies with absolute magnitudes dimmer than H=6 even a dark albedo of 0.04 corresponds to a diameter less than 400 km.^[3]

Brighter than 1

Artistic comparison of Eris, Pluto, Makemake, Haumea, Sedna, 2007 OR₁₀, Quaoar, Orcus, and Earth. ( )

These have all been accepted as dwarf planets by the IAU.

Name	H ^{[citation needed]}	Category	Diameter (km)	Mass (10²⁰ kg)	Average distance from the Sun (AU)^[1]
Eris	−1.19	SDO	2326±12	167	68
Pluto	−0.70	plutino	2306±20	130	39
Makemake	−0.42	cubewano	1478±17	≈30	46
Haumea	0.05	haumeid	1240 +69 −58	40	43

Between 1 and 3

These TNOs would be over a thousand km across, assuming a dark generic albedo of 0.09, and have theoretical minimum diameters of at least 334 km. Brown categorized these with the dwarf planets accepted by the IAU, and Tancredi has recommended to the IAU that they accept them as dwarf planets^[10] (apart from 2007 OR₁₀, which he did not consider).

Name	H ^{[citation needed]}	Category	Diameter (km)	Mass (10²⁰ kg)	Average distance from the Sun (AU)^[1]
Sedna	1.83	detached object	995 ± 80	≈ 10	519
(225088) 2007 OR₁₀	1.92	SDO	1280±210	?	67
Orcus	2.30	plutino	917±25	6.3^[11]	39
Quaoar	2.48	cubewano	1,110±5	14 ± 1	44

Between 3 and 4

These minor planets have theoretical minimum diameters of 213–336 km. Ceres is officially accepted as a dwarf planet.

Name	H^{[citation needed]}	Category	Diameter (km)	Mass (10²⁰ kg)	Average distance from the Sun (AU)^[1]
Vesta	3.20	asteroid	525.4 ± 0.2^[12]	2.59^[13]	2.361
Ixion	3.20	plutino	650 +260 −220	≈3?	39.65
(55636) 2002 TX₃₀₀	3.21	haumeid	286 ± 10	≈0.12	43.11
(55565) 2002 AW₁₉₇	3.26	cubewano	700±50	≈ 4?	47.30
Ceres	3.36	asteroid	950 ± 3	9.43 ± 0.07	2.767
(202421) 2005 UQ₅₁₃	3.40	cubewano	≈920		43
(229762) 2007 UK₁₂₆	3.44	SDO	599 ± 77		73
174567 Varda	3.49	cubewano	≈820		45.94
(55637) 2002 UX₂₅	3.60	cubewano	697 +23 −25	≈3.3?	42.53
Varuna	3.70	cubewano	936 +238 −324^[14]	≈3.7?	42.90
(303775) 2005 QU₁₈₂	3.73	SDO	416 ± 73		113
2010 EK₁₃₉	3.76	SDO	470 +35 −10		69.4
(307261) 2002 MS₄	3.77	cubewano	934 ± 47		41.90
(84522) 2002 TC₃₀₂	3.78	5:2 SDO	584 +106 −88^[15]	≈15?	55.02
2006 QH₁₈₁	3.80	semi-detached	760 (assumed)		67.3
(145452) 2005 RN₄₃	3.85	cubewano	679 +55 −73		41.53
(90568) 2004 GV₉	3.90	cubewano	677 ± 70	1.1–5.0	42.23
2010 KZ₃₉	3.94	SDO	644 (assumed)		45.0
(120178) 2003 OP₃₂	3.95	haumeid	≈ 230		43.24

Between 4 and 5

These minor planets have theoretical minimum diameters of 134–212 km.

Name	H^{[citation needed]}	Category	Diameter (km)			Mass (10²⁰ kg)	Average distance from the Sun (AU)^[1]
Name	H^{[citation needed]}	Category	by ^[1]	by ^[16]	others	Mass (10²⁰ kg)	Average distance from the Sun (AU)^[1]
(145453) 2005 RR₄₃	4.00	haumeid		697	252 km		43
(208996) 2003 AZ₈₄	4.00	plutino	710	686	590–785 km^[17]		39.45
(230965) 2004 XA₁₉₂	4.00	cubewano		696			46.98
(84922) 2003 VS₂	4.01	plutino	629	636	523.0+35.1 −34.4^[18]		39.27
(42301) 2001 UR₁₆₃	4.05	9:4 SDO	620	636			51.40
Pallas	4.13	asteroid			582×556×500±9 km^[8]	2.11±0.26^[19]	2.772
2010 RE₆₄	4.2	cubewano			380–860^[20]		45.8
2010 RF₄₃	4.2	cubewano			380–860^[20]		46.5
120347 Salacia	4.2	cubewano	560	548	854±45^[15]	4.5 ± 0.2	41.97
(175113) 2004 PF₁₁₅	4.2	plutino		505			39.18
2003 UZ₄₁₃	4.3	plutino		591
(120348) 2004 TY₃₆₄	4.3	other TNO	540	554			38.72
(278361) 2007 JJ₄₃	4.43	cubewano	≈ 700		47.99
2010 VR₁₁	4.4	cubewano			350–784^[20]		44.4
2010 FX₈₆	4.4	cubewano		580	350–784^[20]		44.05
2009 YE₇	4.4	SDO			210-584		54.2
2008 ST₂₉₁	4.4	SDO		583	350–784^[20]		106
(145451) 2005 RM₄₃	4.4	SDO	560	580			89.73
2004 NT₃₃	4.4	cubewano		580
2004 XR₁₉₀	4.47	SDO	540	572			57.36
2010 VV₁₁	4.5	cubewano			330–750^[20]		42
(119951) 2002 KX₁₄	4.5	cubewano?	560	560	<560(?)^[17]		39.01
(144897) 2004 UX₁₀	4.5	plutino		529			39.1
(19308) 1996 TO₆₆	4.56	haumeid	540	900	200 km		43.19
2004 PR₁₀₇	4.6	lost	520	522			≈45
2010 VZ₉₈	4.7	cubewano			305–680^[20]		43.2
2001 QF₂₉₈	4.7	plutino	490	420			39.30
(26375) 1999 DE₉	4.7	2:5 TNO	490	461	461±45^[17]	1?	55.72
38628 Huya	4.7	plutino	480	506	532±25^[17]	1.6?	39.76
(145480) 2005 TB₁₉₀	4.7	detached		505			76.38
(47171) 1999 TC₃₆	4.73	plutino	440		A₁=286 +45 −38 A₂=265 +41 −35	0.12^[21]	39.27
2007 JH₄₃	4.7	plutino		522			39.56
2003 QX₁₁₃	4.7	detached	450	505			49.9
(24835) 1995 SM₅₅	4.8	haumeid	470	702	174 km		41.64
(120132) 2003 FY₁₂₈	4.8	detached	430	440			49.77
(82075) 2000 YW₁₃₄	4.8	8:3 TNO	430	431			57.77
19521 Chaos	4.9	cubewano	450	745			45.56
2002 XV₉₃	4.9	plutino	430	457			39.22
2002 CY₂₄₈	4.9	cubewano	410	440			46.18
2008 OG₁₉	4.9	SDO		461			67
2000 CN₁₀₅	5.0	cubewano	430	440			44.65

Probable per Brown

Mike Brown considers the following bodies, ranked by estimated size, to be "probably" plutoids. Asteroids are not considered.

The terms for varying degrees of likelihood are:

Near certainty: Sufficient confidence to say these must be in hydrostatic equilibrium even if predominantly rocky.

Highly likely: Estimated/measured to be over 600 km. The size would have to be "grossly in error" or they would have to be primarily rocky to not be dwarf planets.

Likely: Estimated/measured to be over 500 km. Uncertainties in measurement mean that some of these will be significantly smaller and thus doubtful.

Probable: Estimated/measured to be over 400 km. Expected to be dwarf planets if they are icy and that figure is correct.

All sizes are estimates. Occultation probably gives the most exact estimate. In cases without measurement, the "typical" albedo for an object is assumed from its absolute magnitude, and the size estimate is computed using these values.

Probable plutoids (as of 2014 Jan 18)^[22]
rank	name	diameter (km)	albedo (%)	absolute magnitude (H)	comments	likelihood
1	Eris	2330	99	−1.1	(occultation)	near certainty
2	Pluto	2329	64	−0.7	(occultation)	near certainty
3	Makemake	1426	81	0.1	(occultation)	near certainty
4	2007 OR₁₀	1290	19	2.0	(radiometric)	near certainty
5	Haumea	1252	80	0.4	1920 x 1540 x 990 (inferred:lightcurve, mass, radiometry)	near certainty
6	Quaoar	1092	13	2.7	(radiometric)	near certainty
7	Sedna	1041	32	1.8	(radiometric)	near certainty
8	Orcus	983	23	2.3	(radiometric)	near certainty
9	2002 MS₄	960	5	4.0	(radiometric)	near certainty
10	Salacia	921	4	4.2	(radiometric)	near certainty
11	Varuna	764	9	3.9	(radiometric)	highly likely
12	2003 AZ₈₄	747	11	3.7	(radiometric)	highly likely
13	2002 UX₂₅	704	11	3.9	(radiometric)	highly likely
14	2004 GV₉	703	8	4.2	(radiometric)	highly likely
15	2002 AW₁₉₇	698	12	3.8	(radiometric)	highly likely
16	2005 RN₄₃	697	11	3.9	(radiometric)	highly likely
17	Varda	692	13	3.7	(large/estimated)	highly likely
18	2005 UQ₅₁₃	692	13	3.7	(large/estimated)	highly likely
19	Ixion	674	12	3.8	(radiometric)	highly likely
20	2007 JJ₄₃	614	10	4.2	(large/estimated)	highly likely
21	2007 UK₁₂₆	612	17	3.7	(radiometric)	highly likely
22	Chaos	612	5	5.0	(radiometric)	highly likely
23	2004 XA₁₉₂	600	10	4.3	(large/estimated)	highly likely
24	2010 KZ₃₉	600	10	4.3	(large/estimated)	highly likely
25	2002 TC₃₀₂	591	12	4.2	(radiometric)	likely
26	2010 RF₄₃	586	10	4.4	(large/estimated)	likely
27	2002 XW₉₃	584	4	5.4	(radiometric)	likely
28	2001 UR₁₆₃	572	9	4.5	(large/estimated)	likely
29	2003 UZ₄₁₃	572	9	4.5	(large/estimated)	likely
30	2002 XV₉₃	564	4	5.4	(radiometric)	likely
31	2006 QH₁₈₁	559	9	4.6	(large/estimated)	likely
32	2008 ST₂₉₁	559	9	4.6	(large/estimated)	likely
33	2010 RE₆₄	559	9	4.6	(large/estimated)	likely
34	2010 FX₈₆	559	9	4.6	(large/estimated)	likely
35	2005 RM₄₃	546	9	4.7	(large/estimated)	likely
36	2004 XR₁₉₀	546	9	4.7	(large/estimated)	likely
37	2004 NT₃₃	546	9	4.7	(large/estimated)	likely
38	2003 VS₂	537	15	4.1	(radiometric)	likely
39	2004 TY₃₆₄	533	8	4.8	(large/estimated)	likely
40	2008 OG₁₉	520	8	4.9	(large/estimated)	likely
41	2010 VK₂₀₁	520	8	4.9	(large/estimated)	likely
42	2005 RS₄₃	510	4	5.5	(blue/estimated)	likely
43	2008 AP₁₂₉	508	8	5.0	(large/estimated)	likely
44	2003 QX₁₁₃	508	8	5.0	(large/estimated)	likely
45	2007 JH₄₃	508	8	5.0	(large/estimated)	likely
46	2000 YW₁₃₄	496	7	5.1	(large/estimated)	probably
47	2004 PG₁₁₅	484	7	5.1	(large/estimated)	probably
48	2002 WC₁₉	484	7	5.1	(large/estimated)	probably
49	2007 XV₅₀	484	7	5.1	(large/estimated)	probably
50	2004 PF₁₁₅	482	12	4.5	(radiometric)	probably
51	2010 EK₁₃₉	475	25	3.8	(radiometric)	probably
52	1999 DE₉	474	7	5.2	(radiometric)	probably
53	1998 SN₁₆₅	473	4	5.7	(radiometric)	probably
54	2010 TJ	473	7	5.2	(large/estimated)	probably
55	2010 VZ₉₈	473	7	5.2	(large/estimated)	probably
56	2010 RF₆₄	473	7	5.2	(large/estimated)	probably
57	2011 FW₆₂	473	7	5.2	(large/estimated)	probably
58	2005 TB₁₉₀	469	15	4.4	(radiometric)	probably
59	2002 KX₁₄	468	10	4.9	(radiometric)	probably
60	2003 FY₁₂₈	467	8	5.1	(radiometric)	probably
61	Huya	466	8	5.0	(radiometric)	probably
62	1999 CD₁₅₈	462	6	5.3	(large/estimated)	probably
63	2010 EL₁₃₉	462	6	5.3	(large/estimated)	probably
64	2002 VR₁₂₈	459	5	5.6	(radiometric)	probably
65	2003 QX₁₁₁	453	2	6.8	(radiometric)	probably
66	1996 GQ₂₁	451	6	5.4	(large/estimated)	probably
67	2008 QY₄₀	451	6	5.4	(large/estimated)	probably
68	2006 HH₁₂₃	451	6	5.4	(large/estimated)	probably
69	2010 ET₆₅	451	6	5.4	(large/estimated)	probably
70	2008 NW₄	451	6	5.4	(large/estimated)	probably
71	2008 UA₃₃₂	451	6	5.4	(large/estimated)	probably
72	2010 HE₇₉	451	6	5.4	(large/estimated)	probably
73	2011 GM₂₇	451	6	5.4	(large/estimated)	probably
74	2002 GD₃₂	428	4	5.9	(blue/estimated)	probably
75	2001 QF₂₉₈	421	7	5.4	(radiometric)	probably
76	2005 QU₁₈₂	415	33	3.8	(radiometric)	probably
77	2004 UX₁₀	409	14	4.8	(radiometric)	probably
78	1999 TC₃₆	403	8	5.4	(radiometric)	probably

Another 261 objects were listed as "possible" dwarfs, depending on composition and the accuracy of size and mass estimates.

Probable per Tancredi

Gonzalo Tancredi (2010) presented a report to the IAU evaluating a list of 46 candidates for dwarf-planet status based on light curve amplitude analysis and the assumption that the object is more than 450 km in diameter. Some diameters are measured, some are best-fit estimates, and others use an assumed albedo of 0.10. Of these, he identified 15 as dwarf planets by his criteria, with another nine being considered possible. To be cautious, he advised the IAU to "officially" accept as dwarf planets the top three: Sedna, Orcus, and Quaoar.^[10] Although the IAU had anticipated Tancredi's recommendations, as of 2013 they have not responded.

Probable plutoids (as of 2009)
name	absolute magnitude (H)	diameter (km)	likelihood
Eris	−1.1	2600	accepted (measured)
Pluto	−0.7	2390	accepted (measured)
Makemake	0	1500	accepted
Haumea	0.5	1150	accepted
Sedna	1.8	1600	accepted (and recommended)
Orcus	2.5	946	accepted (and recommended)
Quaoar	2.6	908	accepted (and recommended)
2002 TX₃₀₀	3.49	800^*	accepted
2002 AW₁₉₇	3.61	735	accepted
2003 AZ₈₄	3.71	686	accepted
28978 Ixion	3.84	650	accepted
20000 Varuna	3.99	500	accepted
2004 GV₉	4.2	677	accepted
38628 Huya	5.23	533	accepted
1996 TL₆₆	5.46	575	accepted
174567 Varda	3.6	801^#	possible
2005 RN₄₃	3.9	697^#	possible
2005 RR₄₃	4	666^*	possible
2003 OP₃₂	4.1	636^*	possible
2001 UR₁₆₃	4.2	607^#	possible
2004 SB₆₀	4.2	607^#	possible
2005 RM₄₃	4.4	554^#	possible
2004 UX₁₀	4.5	529^#	possible
1999 DE₉	4.7	482	possible

* In 2009, Mike Brown wrote that 2002 TX₃₀₀ was a Haumea family member with a diameter less than 400 km.^[23] An occultation of a star on on October 9, 2009, produced a diameter of 286 kilometers, indicating an albedo of about 0.88.^[24] 2005 RR₄₃ and 2002 OP₃₂ are also suspected members of the Haumea family, and so are likely to be substantially smaller than the figures here.

# Diameter estimated from assumed albedo.

Spitzer alpha candidates

Calculation of the diameter of Ixion depends on the albedo (the fraction of light that it reflects), which is currently unknown.

In 2007, observations using the Spitzer Space Telescope were used to calculate the sizes of several large TNOs. The following were found to be greater than 600 km in diameter.^[17] (2007 OR₁₀ is not included because it was not observed by Spitzer.) Although (84522) 2002 TC₃₀₂ has a dim absolute magnitude, it is placed high on the list because it was believed to have a low albedo.

Name	(H)	Spitzer Size (km)	Spitzer Albedo	V–R
Eris	−1.1	2,600+400 −200	0.70+0.15 −0.20
Sedna	1.6	<1,600	>0.16	0.78
Makemake	0.0	1,500+400 −200	0.80+0.10 −0.20
Haumea	0.5	1,150+250 −100	0.84+0.10 −0.20
(84522) 2002 TC₃₀₂	3.8	1,145±331	0.03+0.03 −0.01	0.67
Orcus	2.3	946±73	0.20±0.03	0.37
Quaoar	2.5	844±198	0.20+0.13 −0.07	0.64
(55565) 2002 AW₁₉₇	3.2	735±112	0.12+0.04 −0.03	0.56
(84922) 2003 VS₂	4.0	725±193	0.06+0.05 −0.02	0.59
(307261) 2002 MS₄	3.8	726±123	0.08+0.04 −0.02	0.38
(208996) 2003 AZ₈₄	4.0	686±97	0.12+.04 −.03	0.36
(55637) 2002 UX₂₅	3.6	681±115	0.12+0.05 −0.03	0.57
(90568) 2004 GV₉	3.9	677±70	0.08+0.02 −0.01	0.52
Ixion	3.2	573±141	0.16+0.12 −0.06	0.61

References

↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 Mike Brown. "The Dwarf Planets". Retrieved 2008-01-20.
↑ "Today we know of more than a dozen dwarf planets in the solar system [and] it is estimated that the ultimate number of dwarf planets we will discover in the Kuiper Belt and beyond may well exceed 10,000".The PI's Perspective
↑ 3.0 3.1 Dan Bruton. "Conversion of Absolute Magnitude to Diameter for Minor Planets". Department of Physics & Astronomy (Stephen F. Austin State University). Retrieved 2008-06-13.
↑ "IAU 2006 General Assembly: Result of the IAU Resolution votes". International Astronomical Union. 2006. Retrieved 2008-01-26.
↑ "Dwarf Planets". NASA. Retrieved 2008-01-22.
↑ "Plutoid chosen as name for Solar System objects like Pluto" (Press release).
↑ "AstDys (47171) 1999TC36 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2009-12-07.
↑ 8.0 8.1 Savage, Don; Jones, Tammy; and Villard, Ray (1995-04-19). "Asteroid or Mini-Planet? Hubble Maps the Ancient Surface of Vesta". Hubble Site News Release STScI-1995-20. Retrieved 2006-10-17. Cite uses deprecated parameters (help)
↑ "JPL Small-Body Database Search Engine: orbital class (TNO) and H < 6 (mag)". JPL Solar System Dynamics. Retrieved 2013-12-21.
↑ 10.0 10.1 Tancredi, G. (2010). "Physical and dynamical characteristics of icy "dwarf planets" (plutoids)". Icy Bodies of the Solar System: Proceedings IAU Symposium No. 263, 2009.
↑ Brown, M.E.; Ragozzine, D.; Stansberry, J.; Fraser, W.C. (2009). "The size, density, and formation of the Orcus-Vanth system in the Kuiper belt". AJ. arXiv:0910.4784. Bibcode:2010AJ....139.2700B. doi:10.1088/0004-6256/139/6/2700. Cite uses deprecated parameters (help)
↑ Russell, C. T.; et al. (2012). "Dawn at Vesta: Testing the Protoplanetary Paradigm". Science 336 (6082): 684. Bibcode:2012Sci...336..684R. doi:10.1126/science.1219381.
↑ Baer, James; Chesley, Steven R. (2008). "Astrometric masses of 21 asteroids, and an integrated asteroid ephemeris" (PDF). Celestial Mechanics and Dynamical Astronomy (Springer Science+Business Media B.V. 2007) 100 (2008): 27–42. Bibcode:2008CeMDA.100...27B. doi:10.1007/s10569-007-9103-8. Retrieved 2008-11-11. Cite uses deprecated parameters (help)
↑ W. M. Grundy, K. S. Noll, D. C. Stephens (2005). "Diverse albedos of small trans-neptunian objects". Icarus (journal) 176 (1): 184–191. arXiv:astro-ph/0502229. Bibcode:2005Icar..176..184G. doi:10.1016/j.icarus.2005.01.007.
↑ 15.0 15.1 S. Fornasier, E. Lellouch, T. Müller, P. Santos-Sanz, P. Panuzzo, C. Kiss, T. Lim, M. Mommert, D. Bockelée-Morvan, E. Vilenius, J. Stansberry, G.P. Tozzi, S. Mottola, A. Delsanti, J. Crovisier, R. Duffard, F. Henry, P. Lacerda, A. Barucci, & A. Gicquel (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.
↑ Robert Johnston. "List of Known Trans-Neptunian Objects". Retrieved 2010-08-07.
↑ 17.0 17.1 17.2 17.3 17.4 Barucci, M.A.; John Stansberry, Will Grundy, Mike Brown, Dale Cruikshank, John Spencer, David Trilling, Jean-Luc Margot (2007). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope". Kuiper Belt. arXiv:astro-ph/0702538. Bibcode:2008ssbn.book..161S. Cite uses deprecated parameters (help)
↑ Mommert, Michael; Harris, A. W.; Kiss, C.; Pál, A.; Santos-Sanz, P.; Stansberry, J.; Delsanti, A.; Vilenius, E.; Müller, T. G.; Peixinho, N.; Lellouch, E.; Szalai, N.; Henry, F.; Duffard, R.; Fornasier, S.; Hartogh, P.; Mueller, M.; Ortiz, J. L.; Protopapa, S.; Rengel, M.; Thirouin, A. (May 2012). "TNOs are cool: A survey of the trans-Neptunian region—V. Physical characterization of 18 Plutinos using Herschel-PACS observations". Astronomy & Astrophysics 541: A93. arXiv:1202.3657. Bibcode:2012A&A...541A..93M. doi:10.1051/0004-6361/201118562.
↑ Baer, James; Steven R. Chesley (2008). "Astrometric masses of 21 asteroids, and an integrated asteroid ephemeris" (PDF). Celestial Mechanics and Dynamical Astronomy (Springer Science+Business Media B.V. 2007) 100 (2008): 27–42. Bibcode:2008CeMDA.100...27B. doi:10.1007/s10569-007-9103-8. Retrieved 2008-11-11. Cite uses deprecated parameters (help)
↑ 20.0 20.1 20.2 20.3 20.4 20.5 20.6 "Absolute Magnitude (H)". NASA/JPL. Retrieved 2008-12-09.
↑ Benecchi, S.D; Noll, K. S.; Grundy, W. M.; Levison, H. F. (2009). "(47171) 1999 TC36, A Transneptunian Triple". Icarus. arXiv:0912.2074. Bibcode:2010Icar..207..978B. doi:10.1016/j.icarus.2009.12.017. Cite uses deprecated parameters (help)
↑ Mike Brown, How many dwarf planets are there in the outer solar system?
↑ Mike Brown (2009-12-29). "A ghost of Christmas past". Mike Brown's Planets (blog). Retrieved 2009-12-29.
↑ Elliot, J. L.; Person, M. J. et al. (2010). "Size and albedo of Kuiper belt object 55636 from a stellar occultation". Nature 465 (7300): 897–900. Bibcode:2010Natur.465..897E. doi:10.1038/nature09109. PMID 20559381.

External links

How many dwarf planets are there in the outer solar system? (updates daily) (Mike Brown)
Details on the dwarf planet size calculations (Mike Brown)
Which are the Dwarfs in the Solar System? Tancredi,G; Favre,S. Icarus, Volume 195, Issue 2, p. 851–862.
NASA JPL Small-Body Database Search Engine

v t e Dwarf planets

Asteroid belt	Ceres

Kuiper belt	Pluto Makemake Haumea Likely: Orcus Quaoar Ixion Salacia Chaos Varda 2002 AW₁₉₇ 2005 UQ₅₁₃ 2002 UX₂₅ Varuna 2007 JJ₄₃ 2002 MS₄ 2005 RN₄₃ 2004 GV₉ 2003 VS₂ 2003 AZ₈₄ 2004 XA₁₉₂ 2010 RE₆₄ 2010 RF₄₃ 2003 UZ₄₁₃

Scattered disc	Eris Likely: 2007 OR₁₀ 2007 UK₁₂₆ 2005 QU₁₈₂ 2006 QH₁₈₁ 2010 EK₁₃₉ 2002 TC₃₀₂ 2010 KZ₃₉ 2001 UR₁₆₃

Other	Likely: Sedna

See also: Triton List of trans-Neptunian objects List of possible dwarf planets List of Solar System objects List of Solar System objects by size

v t e Trans-Neptunian objects

TNO classes	Cubewanos Scattered-disc objects Detached objects Resonant objects (Neptune trojans Plutinos Twotinos) Natural satellites Double objects

Plutoids & moons	Pluto Charon (Pluto I) Nix (Pluto II) Hydra (Pluto III) Kerberos (Pluto IV) Styx (Pluto V) Haumea Hi'iaka (Haumea I) Namaka (Haumea II) Makemake Eris Dysnomia (Eris I)

v t e The Solar System



The Sun Mercury Venus Earth Mars Ceres Jupiter Saturn Uranus Neptune Pluto Haumea Makemake Eris

Moons Terrestrial Martian Jovian Saturnian Uranian Neptunian Plutonian Haumean Eridian

Rings Jovian Saturnian Uranian Neptunian Rhean

Meteoroids Minor planets Asteroids Asteroid belt Centaurs TNOs Kuiper belt Scattered disc Comets Oort cloud

Astronomical object Star Planet Double planet Dwarf planet Small Solar System body Gas giant Ice giant Planetary system

List of Solar System objects List of Solar System objects by size List of minor planets

Solar System → Local Interstellar Cloud → Local Bubble → Gould Belt → Orion Arm → Milky Way → Milky Way subgroup → Local Group → Virgo Supercluster → Pisces–Cetus Supercluster Complex → Observable universe → Universe Each arrow (→) may be read as "within" or "part of".

PORTALS: Astronomy Earth sciences Solar System

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