List of possible dwarf planets

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

Lua error in package.lua at line 80: module 'strict' not found. 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 (IAU) 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

In 2008, the IAU modified its naming procedures such that objects considered most likely to be dwarf planets receive differing treatment than others. Objects that have an absolute magnitude (H) less than +1 (and hence a minimum diameter of 838 kilometres (521 mi) if the albedo is below 100%^[3]) are overseen by two naming committees, one for minor planets and one for planets. Once named, the objects are declared to be dwarf planets. Makemake and Haumea are the only objects to have proceeded through the naming process as presumed dwarf planets; currently there are no other bodies that meet this criterion. All other bodies are named by the minor-planet naming committee alone, and the IAU has not stated how or if they will be accepted as dwarf planets.

Limiting values

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

The qualifying feature of a dwarf planet is that it "has sufficient mass for its self-gravity to overcome rigid-body forces so that it assumes a hydrostatic equilibrium (nearly round) shape".^[4]^[5]^[6] Current observations are generally insufficient for a direct determination as to whether a body meets this definition. Based on a comparison with the icy moons that have been visited by spacecraft, such as Mimas (round at 400 km in diameter) and Proteus (irregular at 410–440 km in diameter), Michael Brown estimated that an icy body relaxes into hydrostatic equilibrium at a diameter somewhere between 200 and 400 km.^[1]

Ceres is thought to be the only dwarf planet in the asteroid belt. 4 Vesta, the second-most-massive asteroid, appears to have a fully differentiated interior and was therefore in equilibrium at some point in its history, but it is not today.^[7] The third-most massive object, 2 Pallas, has a somewhat irregular surface and is thought to have only a partially differentiated interior. Brown has estimated that, because rocky objects are more rigid than icy objects, rocky objects below 900 kilometres (560 mi) in diameter may not be in hydrostatic equilibrium and thus not dwarf planets.^[1]

After Brown and Tancredi made their calculations, it was discovered that Iapetus (1,470 km in diameter) and smaller moons of Saturn with well-determined shapes are not in hydrostatic equilibrium as had been thought. They have a hydrostatic shape that froze in some time ago and that does not match the shape an equilibrium body would have at their current rotation rates.^[8] Ceres, at 950 km, is the smallest body for which detailed measurements are consistent with hydrostatic equilibrium. ^[9] It is not clear whether trans-Neptunian objects would behave more like Ceres or Iapetus; thus, some or all trans-Neptunian dwarf planets smaller than Pluto and Eris might not actually be in equilibrium.^{[citation needed]} The IAU has not addressed the issue since these findings.

Tancredi's assessment

In 2010, Gonzalo Tancredi 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 was more than 450 kilometres (280 mi) 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 had not responded.

Brown's assessment

Brown's categories	Min. ⌀	Number of objects
nearly certainly	>900 km	10
highly likely	600–900 km	16
likely	500–600 km	23
probably	400–500 km	47
possibly	200–400 km	298
Source: Mike Brown,^[11] as of April 10, 2016. (Summary figures differ on M. Brown's website using a cumulative count).

Mike Brown considers a large number of trans-Neptunian bodies, ranked by estimated size, to be "probably" dwarf planets.^[11] He did not consider asteroids, stating "In the asteroid belt Ceres, with a diameter of 900 km, is the only object large enough to be round".^[11]

The terms for varying degrees of likelihood he split these into:

Near certainty: diameter estimated/measured to be over 900 kilometres (560 mi). Sufficient confidence to say these must be in hydrostatic equilibrium, even if predominantly rocky.
Highly likely: diameter estimated/measured to be over 600 kilometres (370 mi). The size would have to be "grossly in error" or they would have to be primarily rocky to not be dwarf planets.
Likely: diameter estimated/measured to be over 500 kilometres (310 mi). Uncertainties in measurement mean that some of these will be significantly smaller and thus doubtful.
Probable: diameter estimated/measured to be over 400 kilometres (250 mi). Expected to be dwarf planets, if they are icy, and that figure is correct.
Possible: diameter estimated/measured to be over 200 kilometres (120 mi). Icy moons transition from a round to irregular shape in the 200–400 km range, suggesting that the same figure holds true for KBOs. Thus, some of these objects could be dwarf planets.
Probably not: diameter estimated/measured to be under 200 km. No icy moon under 200 km is round, suggesting that the same is true for KBOs. The estimated size of these objects would have to be in error for them to be dwarf planets.

Likeliest dwarf planets

The following trans-Neptunian objects have estimated diameters at least 300 kilometres (190 mi) and so may be dwarf planets. Not all bodies estimated to be this size are included. The list is complicated by bodies such as (47171) 1999 TC36 that were at first assumed to be large single objects but later discovered to be binary or triple systems of smaller bodies.^[12] The asteroid Ceres is added for comparison.

The default sort is per Brown's size estimate. The IAU-recognised dwarf planets have bold names. Brown's diameter estimates are in red when they are based upon an assumed albedo. Explanations and sources for the measured masses and diameters can be found in the corresponding articles linked in column "Body" of the table.

Body	Per Brown^[11]			Measured			per measured	Diameter per assumed albedo		Result per Tancredi^[10]	Category	Best^{[lower-alpha 1]} diameter (km)
Body	H	Diameter^{[lower-alpha 2]} (km)	Geometric albedo (%)	Mass (10¹⁸kg)	H ^[13]^[14]	Diameter (km)	Geometric albedo^{[lower-alpha 3]} (%)	Small albedo=100% (km)	Large albedo=4% (km)	Result per Tancredi^[10]	Category	Best^{[lower-alpha 1]} diameter (km)
Eris	−1.1	2330	99	16700	−1.2	2326±12	99	2310	11548	accepted (measured)	SDO	2326
Pluto	−0.7	2329	64	13030	−0.4	2374±8	45	1598	7989	accepted (measured)	2:3 resonant	2374
Makemake	0.1	1426	81		−0.3	1430±14	114	1526	7629	accepted	cubewano	1430
(225088) 2007 OR10	2	1290	19		2.5	1535+75 −225	7	420	2101		SDO	1535
Haumea	0.4	1252	80	4000	0.1	1430	79	1269	6346	accepted	cubewano	1430
Quaoar	2.7	1092	13	1400	2.82	1110±5	11	363	1813	accepted (and recommended)	cubewano	1110
Sedna	1.8	1041	32		1.83	995±80	33	572	2861	accepted (and recommended)	detached	995
Orcus	2.3	983	23	580	2.31	917±25	25	459	2293	accepted (and recommended)	2:3 resonant	917
(307261) 2002 MS4	4	960	5		3.7	934±47	7	242	1209		cubewano	934
Ceres				939	3.36	946±2	9	283	1414		asteroid belt	946
Salacia	4.2	921	4	450	4.25	854±45	5	188	939	possible	cubewano	854
Varuna	3.9	783	9		3.76	668+154 −86	12	235	1176	accepted	cubewano	668
2013 FY27	3.3	772	15		3			334	1669		SDO	772
(208996) 2003 AZ84	3.7	747	11		3.74	727+62 −67	11	237	1187	accepted	2:3 resonant	727
(55565) 2002 AW197	3.8	716	12		3.5	768+39 −38	12	265	1326	accepted	cubewano	768
(55637) 2002 UX25	3.9	704	11	125	3.87	665±29	11	224	1118		cubewano	665
(90568) 2004 GV9	4.2	703	8		4.25	680±34	8	188	939	accepted	3:5 resonant	680
Varda	3.7	702	13	265	3.61	705+81 −75	13	252	1260	possible	cubewano	705
(202421) 2005 UQ513	3.7	702	13		3.4	498+63 −75	31	278	1388		cubewano	498
(145452) 2005 RN43	3.9	697	11		3.89	679+55 −73	11	222	1108	possible	cubewano	679
Ixion	3.8	674	12		3.83	617+19 −20	14	228	1139	accepted	2:3 resonant	617
(278361) 2007 JJ43	4.1	622	11		3.9			221	1103		cubewano	622
2015 KH162	4.1	622	11		3.9			221	1103		detached	622
(229762) 2007 UK126	3.7	612	17		3.69	599±77	16	243	1215		SDO	599
Chaos	5	612	5		4.8	600+140 −130	6	146	729		cubewano	600
2012 VP113	4.2	608	10		4			211	1053		detached	608
2010 KZ39	4.2	608	10		4			211	1053		cubewano	608
2010 RF43	4.3	593	10		4.1			201	1006		SDO	593
2013 FZ27	4.3	593	10		4.1			201	1006		cubewano	593
(230965) 2004 XA192	4.3	593	10		4.1	339+120 −95	35	201	1006		1:2 resonant	339
(84522) 2002 TC302	4.2	591	12		3.8	584+106 −88	16	231	1155		2:5 resonant	584
(78799) 2002 XW93	5.4	584	4		5.5			106	528		SDO	584
2008 ST291	4.4	579	9		4.2			192	960		detached	579
2010 FX86	4.4	579	9		4.2			192	960		cubewano	579
2010 RE64	4.5	565	9		4.3			183	917		SDO	565
2004 XR190	4.5	565	9		4.3			183	917		detached	565
2006 QH181	4.5	565	9		4.3			183	917		SDO	565
2002 XV93	5.4	564	4		5.42	549+22 −23	4	110	548		2:3 resonant	549
(455502) 2003 UZ413	4.6	552	9		4.4			175	876		2:3 resonant	552
(145451) 2005 RM43	4.6	552	9		4.4			175	876	possible	SDO	552
2007 XV50	4.7	539	8		4.5			167	837		cubewano	539
2007 JH43	4.7	539	8		4.5			167	837		2:3 resonant	539
(42301) 2001 UR163	4.7	539	8		4.5			167	837	possible	SDO	539
(84922) 2003 VS2	4.1	537	15		4.1	523+35 −34	15	201	1006		2:3 resonant	523
2010 VK201	4.8	526	8		4.6			160	799		cubewano	526
2014 FC69	4.8	526	8		4.6			160	799		detached	526
(444030) 2004 NT33	4.9	514	8		4.7	423+87 −80	13	153	763		cubewano	423
2003 QX113	4.9	514	8		4.7			153	763		SDO	514
(307982) 2004 PG115	5	501	7		4.8			146	729		SDO	501
2014 FT71	5	501	7		4.8			146	729		4:7 resonant	501
(307616) 2003 QW90	5.6	497	4		5.4			111	553		cubewano	497
(119979) 2002 WC19	5.1	490	7		4.9			139	696		1:2 resonant	490
(82075) 2000 YW134	5.1	490	7		4.9			139	696		detached	490
2014 UM33	5.1	490	7		4.9			139	696		cubewano	490
(175113) 2004 PF115	4.5	482	12		4.54	406+98 −75	16	164	821		2:3 resonant	406
(120348) 2004 TY364	5.2	478	7		4.52	512+37 −40	10	166	829		2:3 resonant	512
2008 OG19	5.2	478	7		5			133	665		SDO	478
2011 FW62	5.2	478	7		5			133	665		2:3 resonant	478
2010 TJ	5.2	478	7		5			133	665		SDO	478
2010 RF64	5.2	478	7		5			133	665		cubewano	478
2015 FG345	5.2	478	7		5			133	665		3:5 resonant	478
2010 EK139	3.8	475	25		3.8	470+35 −10	24	231	1155		SDO	470
(26375) 1999 DE9	5.2	474	7		5	461±45	8	133	665	possible	SDO	461
(35671) 1998 SN165	5.7	473	4		5.6	393+39 −38	7	101	504		cubewano	393
(145480) 2005 TB190	4.4	469	15		4.4	464±62	14	175	876		detached	464
(119951) 2002 KX14	4.9	468	10		4.86	445±27	10	142	709		2:3 resonant	445
(120132) 2003 FY128	5.1	467	8		4.8	460±21	10	146	729		SDO	460
1999 CD158	5.3	467	7		5.1			127	635		4:7 resonant	467
2010 EL139	5.3	467	7		5.1			127	635		2:3 resonant	467
2010 HE79	5.3	467	7		5.1			127	635		2:3 resonant	467
(445473) 2010 VZ98	5.3	467	7		5.1			127	635		SDO	467
Huya	5	466	8		5.04	406±16	10	130	652	accepted	2:3 resonant	406
(84719) 2002 VR128	5.6	459	5		5.58	449+42 −43	5	102	509		2:3 resonant	449
(26181) 1996 GQ21	5.4	456	6		5.2			121	606		SDO	456
2013 JW63	5.4	456	6		5.2			121	606		1:2 resonant	456
2011 GM27	5.4	456	6		5.2			121	606		cubewano	456
2010 ET65	5.4	456	6		5.2			121	606		SDO	456
2008 NW4	5.4	456	6		5.2			121	606		cubewano	456
(305543) 2008 QY40	5.4	456	6		5.2			121	606		SDO	456
2008 UA332	5.4	456	6		5.2			121	606		cubewano	456
(315530) 2008 AP129	5.4	456	6		5.2			121	606		cubewano	456
2005 CA79	5.4	456	6		5.2			121	606		1:2 resonant	456
2013 FC28	5.4	456	6		5.2			121	606		cubewano	456
2014 FY71	5.4	456	6		5.2			121	606		SDO	456
2003 QX111	6.8	453	2		6.8			58	290		2:3 resonant	453
2006 HH123	5.4	452	6		5.2			121	606		2:5 resonant	452
(308379) 2005 RS43	5.5	445	6		5.3			116	579		1:2 resonant	445
2010 JK124	5.5	445	6		5.3			116	579		2:3 resonant	445
2010 RO64	5.5	445	6		5.3			116	579		cubewano	445
2010 VW11	5.5	445	6		5.3			116	579		SDO	445
2003 UA414	5.5	445	6		5.3			116	579		cubewano	445
2002 CY248	5.5	445	6		5.3			116	579		cubewano	445
2002 PJ149	5.5	445	6		5.3			116	579		cubewano	445
2001 QF298	5.4	421	7		5.43	408+40 −45	7	109	545		2:3 resonant	408
(437915) 2002 GD32	6	416	4		5.8			92	460		cubewano	416
(303775) 2005 QU182	3.8	415	33		3.8	416±73	31	231	1155		SDO	416
(144897) 2004 UX10	4.8	409	14		4.75	361+124 −94	17	149	746	possible	2:3 resonant	361
1999 CL119	6.2	381	4		6			84	419		cubewano	381
(48639) 1995 TL8	5.6	368	8		5.4			111	553		detached	368
2001 QS297	5.6	368	8		5.4			111	553		cubewano	368
2010 VR11	5.6	368	8		5.4			111	553		cubewano	368
2011 JF31	5.6	368	8		5.4			111	553		cubewano	368
2010 TR19	5.6	368	8		5.4			111	553		SDO	368
2010 ER65	5.6	368	8		5.4			111	553		detached	368
2014 QS441	5.6	368	8		5.4			111	553		cubewano	368
2001 QX322	6.3	364	4		6.1			80	400		SDO	364
2000 KK4	6.3	364	4		6.1			80	400		cubewano	364
2000 PE30	6.3	364	4		6.1			80	400		SDO	364
(82155) 2001 FZ173	6.3	364	4		6.1			80	400		SDO	364
2000 CQ105	6.3	364	4		6.1			80	400		SDO	364
(126154) 2001 YH140	5.7	352	8		5.8	345±45	7	92	460		3:5 resonant	345
2002 GH32	5.7	352	8		5.5			106	528		3:5 resonant	352
2002 XH91	5.7	352	8		5.5			106	528		cubewano	352
(312645) 2010 EP65	5.7	352	8		5.5			106	528		1:2 resonant	352
2013 FB28	5.7	352	8		5.5			106	528		cubewano	352
(444745) 2007 JF43	5.7	352	8		5.5			106	528		2:3 resonant	352
2008 CT190	5.7	352	8		5.5			106	528		SDO	352
2007 PS45	5.7	352	8		5.5			106	528		cubewano	352
2007 TG422	6.4	348	4		6.2			76	382		SDO	348
(15874) 1996 TL66	5.4	344	11		5.4	339±20	11	111	553	accepted	SDO	339
(135182) 2001 QT322	6.4	342	4		6.2			76	382		cubewano	342
2010 AH2	5.8	337	8		5.6			101	504		1:2 resonant	337
2012 XR157	5.8	337	8		5.6			101	504		1:2 resonant	337
2013 RM98	5.8	337	8		5.6			101	504		cubewano	337
2011 HP83	5.8	337	8		5.6			101	504		SDO	337
2010 TY53	5.8	337	8		5.6			101	504		2:3 resonant	337
2010 RN64	5.8	337	8		5.6			101	504		cubewano	337
2010 PK66	5.8	337	8		5.6			101	504		cubewano	337
2010 PU75	5.8	337	8		5.6			101	504		SDO	337
(82158) 2001 FP185	6.4	336	5		6.38	332+31 −24	4	70	352		SDO	332
2001 QC298	6.5	333	4		6.3			73	365		cubewano	333
(148209) 2000 CR105	6.5	333	4		6.3			73	365		detached	333
2001 KA77	5.6	324	10		5			133	665		cubewano	324
2001 XD255	5.9	322	8		5.7			96	481		2:3 resonant	322
2001 RU143	5.9	322	8		5.7			96	481		2:3 resonant	322
(79978) 1999 CC158	5.9	322	8		5.7			96	481		SDO	322
(307251) 2002 KW14	5.9	322	8		5			133	665		cubewano	322
2003 UB292	5.9	322	8		5.7			96	481		cubewano	322
2010 FC49	5.9	322	8		5.7			96	481		2:3 resonant	322
2010 VQ11	5.9	322	8		5.7			96	481		cubewano	322
2014 WT69	5.9	322	8		5.7			96	481		detached	322
2004 VN112	6.6	318	4		6.4			70	349		detached	318
2004 OJ14	6.6	318	4		6.4			70	349		2:5 resonant	318
(168703) 2000 GP183	6.6	318	4		6.4			70	349		2:3 resonant	318
2007 OC10	5.4	315	13		5.7			96	481		SDO	315
2007 TB418	6	308	8		5.8			92	460		2:5 resonant	308
2007 LF38	6	308	8		5.8			92	460		SDO	308
2007 VK305	6	308	8		5.8			92	460		SDO	308
2011 UT410	6	308	8		5.8			92	460		2:3 resonant	308
2013 JH64	6	308	8		5.8			92	460		SDO	308
2000 AF255	6	308	8		5.8			92	460		SDO	308
(150642) 2001 CZ31	6	308	8		5.8			92	460		cubewano	308
2002 GF32	6	308	8		5.8			92	460		2:3 resonant	308
2014 UH192	6	308	8		5.8			92	460		SDO	308
2014 FV71	6	308	8		5.8			92	460		2:5 resonant	308
2000 CP104	6.7	305	4		6.5			67	333		cubewano	305
2005 SD278	6.7	305	4		6.5			67	333		2:5 resonant	305

↑ The measured diameter, else Brown's estimated diameter, else the diameter calculated from H using an assumed albedo of 8%.
↑ Diameters with the text in red indicate that Brown's bot derived them from heuristically expected albedo.
↑ The geometric albedo $A$ is calculated from the measured absolute magnitude $H$ and measured diameter $D$ via the formula: $A =\left ( \frac{1329\times10^{-H/5}}{D} \right ) ^2$

References

↑ ^1.0 ^1.1 ^1.2 Lua error in package.lua at line 80: module 'strict' not found.
↑ "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
↑ Lua error in package.lua at line 80: module 'strict' not found.
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↑ Lua error in package.lua at line 80: module 'strict' not found.
↑ Lua error in package.lua at line 80: module 'strict' not found.
↑ [1]
↑ http://www.planetary.org/blogs/emily-lakdawalla/2015/dps15-1112-ceres.html
↑ ^10.0 ^10.1 Lua error in package.lua at line 80: module 'strict' not found.
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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

[best_diam-13] The measured diameter, else Brown's estimated diameter, else the diameter calculated from H using an assumed albedo of 8%.

[brown_albedo-14] Diameters with the text in red indicate that Brown's bot derived them from heuristically expected albedo.

[albedo-17] The geometric albedo $A$ is calculated from the measured absolute magnitude $H$ and measured diameter $D$ via the formula: $A =\left ( \frac{1329\times10^{-H/5}}{D} \right ) ^2$

[Brown-1] 1.0 ^1.1 ^1.2 Lua error in package.lua at line 80: module 'strict' not found.

[Stern2012-2] "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

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[8] [1]

[9] ttp://www.planetary.org/blogs/emily-lakdawalla/2015/dps15-1112-ceres.html

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v t e Dwarf planets
Asteroid belt	IAU: Ceres No longer rounded and therefore not dwarf planets: Vesta (disrupted out of equilibrium)
Centaurs	Possibly: Chariklo Chiron
Centaurs (extended)	Possibly: 1995 SN55 Ceto 2010 TY53
Plutinos	IAU: Pluto Additional objects proposed by Brown and Tancredi: Orcus Ixion 2003 AZ₈₄ 2004 UX₁₀ Huya Possibly: 2003 UZ₄₁₃ 2003 VS₂ 2002 VR₁₂₈ 2004 PF₁₁₅ 2002 XV93 2007 JH43 2001 QF298
Twotinos	Possibly: 2002 WC₁₉
Other resonances/ unknown resonances:	IAU: Haumea Possibly: 2002 XW₉₃ 1999 DE₉ 1999 KR₁₆ 2001 YH₁₄₀ 2011 GM27 2010 VK201 2013 FZ27 2014 UM33 1999 CD158
Cubewanos:	IAU: Makemake Additional objects proposed by Brown and Tancredi: 2002 MS₄ Salacia Quaoar Varuna Varda 2004 GV₉ 2002 AW₁₉₇ 2002 TX₃₀₀ 2005 RR₄₃ 2003 OP₃₂ 2005 RN₄₃ Possibly: Chaos Altjira Sila-Nunam 2002 UX₂₅ 2007 JJ₄₃ 2005 UQ₅₁₃ 2004 TY₃₆₄ 2003 QW₉₀ 1998 SN₁₆₅ 2002 KX₁₄ Praamzius 2004 NT₃₃ 2010 FX86 2002 CY248 2010 VR11 Rhadamanthus
Scattered disc	IAU: Eris Additional objects proposed by Brown and Tancredi: 2007 OR₁₀ 1996 TL₆₆ 2001 UR₁₆₃ 2005 RM₄₃ Possibly: 2002 TC₃₀₂ 2004 XA₁₉₂ 2005 QU₁₈₂ 2006 QH181 2007 UK₁₂₆ 2010 EK139 2010 KZ39 2010 RE64 2010 RF43 2010 TJ 2013 FY27 2008 OG19 1996 GQ₂₁ 2012 HH₂ 1999 CC₁₅₈ 2006 HH123 2010 VZ98
Area uncertain	Captured satellites that were once dwarf planets: Triton (captured by Neptune) Phoebe (captured by Saturn, and was then disrupted out of equilibrium) Possibly: 2011 FW62 (lost) 2000 YW₁₃₄ V774104
Detached objects	Possibly: 2004 XR190 2010 GB174 2008 ST291 1995 TL₈ 2005 TB₁₉₀ 2003 QX113 2003 FY₁₂₈ 2004 VN112 2000 CR₁₀₅
Sednoids	Objects proposed by Brown and Tancredi: Sedna Possibly: 2012 VP113
Former candidates	Pallas Vesta Hygiea Cybele
See also: Charon Vanth Dysnomia Hiʻiaka Mesoplanet Planemo List of trans-Neptunian objects List of possible dwarf planets List of Solar System objects List of Solar System objects by size

v t e Trans-Neptunian objects
TNO classes	Cubewanos Scattered-disc objects Detached objects Resonant objects (Neptune trojans Plutinos Twotinos) Natural satellites Double objects
Dwarf Planets (moons)	Pluto Charon Styx Nix Kerberos Hydra Haumea Namaka Hi'iaka Makemake S/2015 (136472) 1 Eris Dysnomia
Sednoids	90377 Sedna 2012 VP113

List of possible dwarf planets

Contents

IAU naming procedures

Limiting values

Tancredi's assessment

Brown's assessment

Likeliest dwarf planets

See also

References

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