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Parts-per-million chart of the relative mass distribution of the Solar System, each cubelet denoting 2×1024 kg

This article includes a list of the most massive known objects of the Solar System and partial lists of smaller objects by observed mean radius. These lists can be sorted according to an object's radius and mass and, for the most massive objects, volume, density, and surface gravity, if these values are available.

These lists contain the Sun, the planets, dwarf planets, many of the larger small Solar System bodies (which includes the asteroids), all named natural satellites, and a number of smaller objects of historical or scientific interest, such as comets and near-Earth objects.

Many trans-Neptunian objects (TNOs) have been discovered; in many cases their positions in this list are approximate, as there is frequently a large uncertainty in their estimated diameters due to their distance from Earth.

Solar System objects more massive than 1021 kilograms are known or expected to be approximately spherical. Astronomical bodies relax into rounded shapes (spheroids), achieving hydrostatic equilibrium, when their own gravity is sufficient to overcome the structural strength of their material. It was believed that the cutoff for round objects is somewhere between 100 km and 200 km in radius if they have a large amount of ice in their makeup;[1] however, later studies revealed that icy satellites as large as Iapetus (1,470 kilometers in diameter) are not in hydrostatic equilibrium at this time,[2] and a 2019 assessment suggests that many TNOs in the size range of 400–1,000 kilometers may not even be fully solid bodies, much less gravitationally rounded.[3] Objects that are ellipsoids due to their own gravity are here generally referred to as being "round", whether or not they are actually in equilibrium today, while objects that are clearly not ellipsoidal are referred to as being "irregular."

Spheroidal bodies typically have some polar flattening due to the centrifugal force from their rotation, and can sometimes even have quite different equatorial diameters (scalene ellipsoids such as Haumea). Unlike bodies such as Haumea, the irregular bodies have a significantly non-ellipsoidal profile, often with sharp edges.

There can be difficulty in determining the diameter (within a factor of about 2) for typical objects beyond Saturn. (See 2060 Chiron as an example) For TNOs there is some confidence in the diameters, but for non-binary TNOs there is no real confidence in the masses/densities. Many TNOs are often just assumed to have Pluto's density of 2.0 g/cm3, but it is just as likely that they have a comet-like density of only 0.5 g/cm3.[4]

For example, if a TNO is incorrectly assumed to have a mass of 3.59×1020 kg based on a radius of 350 km with a density of 2 g/cm3 but is later discovered to have a radius of only 175 km with a density of 0.5 g/cm3, its true mass would be only 1.12×1019 kg.

The sizes and masses of many of the moons of Jupiter and Saturn are fairly well known due to numerous observations and interactions of the Galileo and Cassini orbiters; however, many of the moons with a radius less than ~100 km, such as Jupiter's Himalia, have far less certain masses.[5] Further out from Saturn, the sizes and masses of objects are less clear. There has not yet been an orbiter around Uranus or Neptune for long-term study of their moons. For the small outer irregular moons of Uranus, such as Sycorax, which were not discovered by the Voyager 2 flyby, even different NASA web pages, such as the National Space Science Data Center[6] and JPL Solar System Dynamics,[5] give somewhat contradictory size and albedo estimates depending on which research paper is being cited.

There are uncertainties in the figures for mass and radius, and irregularities in the shape and density, with accuracy often depending on how close the object is to Earth or whether it has been visited by a probe.

Graphical overview[edit]

  • Relative diameters of the fifty largest bodies in the Solar System, colored by orbital region. Values are diameters in kilometers. Scale is linear.
    Relative diameters of the fifty largest bodies in the Solar System, colored by orbital region. Values are diameters in kilometers. Scale is linear.
  • Relative masses of the bodies of the Solar System. Objects smaller than Saturn are not visible at this scale.
    Relative masses of the bodies of the Solar System. Objects smaller than Saturn are not visible at this scale.
  • Relative masses of the Solar planets. Jupiter at 71% of the total and Saturn at 21% dominate the system.
    Relative masses of the Solar planets. Jupiter at 71% of the total and Saturn at 21% dominate the system.
  • Relative masses of the solid bodies of the Solar System. Earth at 48% and Venus at 39% dominate. Bodies less massive than Pluto are not visible at this scale.
    Relative masses of the solid bodies of the Solar System. Earth at 48% and Venus at 39% dominate. Bodies less massive than Pluto are not visible at this scale.
  • Relative masses of the rounded moons of the Solar System. Mimas, Enceladus, and Miranda are too small to be visible at this scale.
    Relative masses of the rounded moons of the Solar System. Mimas, Enceladus, and Miranda are too small to be visible at this scale.

Objects with radius over 400 km[edit]

The following objects have a mean radius of at least 400 km. It was once expected that any icy body larger than approximately 200 km in radius was likely to be in hydrostatic equilibrium (HE).[7] However, Ceres (r = 470 km) is the smallest body for which detailed measurements are consistent with hydrostatic equilibrium,[8] whereas Iapetus (r = 735 km) is the largest icy body that has been found to not be in hydrostatic equilibrium.[9] The known icy moons in this range are all ellipsoidal (except Proteus), but trans-Neptunian objects up to 450–500 km radius may be quite porous.[10]

For simplicity and comparative purposes, the values are manually calculated assuming that the bodies are all spheres. The size of solid bodies does not include an object's atmosphere. For example, Titan looks bigger than Ganymede, but its solid body is smaller. For the giant planets, the "radius" is defined as the distance from the center at which the atmosphere reaches 1 bar of atmospheric pressure.[11]

Because Sedna and 2002 MS4 have no known moons, directly determining their mass is impossible without sending a probe (estimated to be from 1.7x1021 to 6.1×1021 kg for Sedna[12]).

Body[note 1] Image Radius[note 2] Volume Mass Surface area Density Gravity[note 3] Type Discovery
(km) (R🜨) (109 km3) (V🜨) (1021 kg) (M🜨) (106 km2) 🜨 (g/cm3) (m/s2) (🜨)
Sun
695508 ± ?[13] 109.2[13] 1,409,300,000[13] 1,301,000[13] 1989100000[13] 333,000[13] 6,078,700[13] 11,918[13] 1.409[13] 274.0[13] 27.94[13] G2V-class star prehistoric
Jupiter
69911±6[14] 10.97 1,431,280 1,321 1898187±88[14] 317.83 61,419[15] 120.41 1.3262±0.0003[14] 24.79[14] 2.528 gas giant planet; has rings prehistoric
Saturn
58232±6[14]
(136775 for A Ring) 		9.140 827,130 764 568317±13[14] 95.162 42,612[16] 83.54 0.6871±0.0002[14] 10.44[14] 1.065 gas giant planet; has rings prehistoric
Uranus
25362±7[14] 3.981 68,340 63.1 86813±4[14] 14.536 8083.1[17] 15.85 1.270±0.001[14] 8.87[14] 0.886 ice giant planet; has rings 1781
Neptune
24622±19[14] 3.865 62,540 57.7 102413±5[14] 17.147 7618.3[18] 14.94 1.638±0.004[14] 11.15[14] 1.137 ice giant planet; has rings 1846
Earth
6371.0±0.0001[14] 1 1,083.21 1 5972.4±0.3[14] 1 510.06447[19] 1 5.5136±0.0003[14] 9.81[14] 1 terrestrial planet prehistoric
Venus
6052±1[14] 0.9499 928.43 0.857 4867.5±0.2[14] 0.815 460.2[20] 0.903 5.243±0.003[14] 8.87[14] 0.905 terrestrial planet prehistoric
Mars
3389.5±0.2[14] 0.5320 163.18 0.151 641.71±0.03[14] 0.107 144.37[21] 0.283 3.9341±0.0007[14] 3.71[14] 0.379 terrestrial planet prehistoric
Ganymede
Jupiter III
2634.1±0.3 0.4135 76.30 0.0704 148.2 0.0248 86.999[22] 0.171 1.936 1.428 0.146 moon of Jupiter (icy) 1610
Titan
Saturn VI
2574.73±0.09[23] 0.4037[a] 71.50 0.0658 134.5 0.0225 83.3054[24] 0.163 1.880±0.004 1.354 0.138 moon of Saturn (icy) 1655
Mercury
2439.4±0.1[14] 0.3829 60.83 0.0562 330.11±0.02[14] 0.0553 74.797[25] 0.147 5.4291±0.007[14] 3.70[14] 0.377 terrestrial planet prehistoric
Callisto
Jupiter IV
2410.3±1.5[23] 0.3783 58.65 0.0541 107.6 0.018 73.005[26] 0.143 1.834±0.003 1.23603 0.126 moon of Jupiter (icy) 1610
Io
Jupiter I
1821.6±0.5[5] 0.2859 25.32 0.0234 89.32 0.015 41.698[27] 0.082 3.528±0.006 1.797 0.183 moon of Jupiter (terrestrial) 1610
Moon
Earth I
1737.5±0.1[28] 0.2727 21.958 0.0203 73.46[29] 0.0123 37.937[30] 0.074 3.344±0.005[28] 1.625 0.166 moon of Earth (terrestrial) prehistoric
Europa
Jupiter II
1560.8±0.5[5] 0.2450 15.93 0.0147 48.00 0.008035 30.613[31] 0.06 3.013±0.005 1.316 0.134 moon of Jupiter (terrestrial) 1610
Triton
Neptune I
1353.4±0.9[a][23] 0.2124[a] 10.38 0.0096 21.39±0.03 0.003599 23.018[32] 0.045 2.061 0.782 0.0797 moon of Neptune (icy) 1846
Pluto
134340
1188.3±0.8 0.187 7.057 0.00651 13.03±0.03 0.0022 17.79 0.034 1.854±0.006 0.620 0.063 dwarf planet; plutino; multiple 1930
Eris
136199
1163±6[b][33] 0.1825[b] 6.59 0.0061 16.6±0.2[34] 0.0028 17 0.033 2.52±0.07 0.824 0.083 dwarf planet; SDO; binary 2003
Haumea
136108
798±6 to 816[35] 0.12 1.98[c] 0.0018 4.01±0.04[36] 0.00066 8.14 0.016 2.018[37][d] 0.401 0.0409 dwarf planet;
resonant KBO (7:12);
trinary; has rings 		2004
Titania
Uranus III
788.9±1.8[23] 0.1237[e] 2.06 0.0019 3.40±0.06 0.00059 7.82[38] 0.015 1.711±0.005 0.378 0.0385 moon of Uranus 1787
Rhea
Saturn V
763.8±1.0[e] 0.1199[e] 1.87 0.0017 2.307 0.00039 7.34[39] 0.014 1.236±0.005 0.26 0.027 moon of Saturn 1672
Oberon
Uranus IV
761.4±2.6[a][23] 0.1195[a] 1.85 0.0017 3.08±0.09 0.0005 7.285[40] 0.014 1.63±0.05 0.347 0.035 moon of Uranus 1787
Iapetus
Saturn VIII
735.6±1.5[5] 0.1153 1.66 0.0015 1.806 0.00033 6.8 0.013 1.088±0.013 0.223 0.0227 moon of Saturn 1671
Makemake
136472
715+19
−11[41] 		0.112 1.53 0.0014 ≈ 3.1 0.00053 6.4 0.013 ≈ 2.1 0.57 0.0581 dwarf planet; cubewano 2005
Gonggong
225088
615±25[42] 0.0983 1.03 0.0009 1.75±0.07 0.00029 4.753 0.009 1.72±0.16 0.3 0.0306 dwarf planet?; resonant SDO (3:10) 2007
Charon
Pluto I
606.0±0.5 0.0951 0.932 0.0009 1.586±0.015 0.00025 4.578[43] 0.009 1.70±0.02 0.288 0.0294 moon of Pluto 1978
Umbriel
Uranus II
584.7±2.8[23] 0.0918 0.837 0.0008 1.28±0.03 0.00020 4.3[44] 0.008 1.39±0.16 0.234 0.024 moon of Uranus 1851
Ariel
Uranus I
578.9±0.6[23] 0.0909 0.813 0.0007 1.25±0.02 0.000226 4.211[45] 0.008 1.66±0.15 0.269 0.027 moon of Uranus 1851
Dione
Saturn IV
561.7±0.45[23] 0.0881 0.741 0.0007 1.095 0.000183 3.965[46] 0.008 1.478±0.003 0.232 0.0237 moon of Saturn 1684
Quaoar
50000
543±2 0.0879 0.737 0.0007 1.20±0.05[47] 0.0002 3.83 0.008 2.0±0.5[48] 0.3 0.0306 cubewano; binary 2002
Tethys
Saturn III
533.0±0.7[23] 0.0834 0.624 0.0006 0.617 0.000103 3.57[49] 0.007 0.984±0.003[50] 0.145 0.015 moon of Saturn 1684
Sedna
90377
498±40 0.0785 0.516 0.0005 sednoid; detached object 2003
Ceres
1
469.7±0.1[51] 0.0742 0.433 0.0004 0.938[52] 0.000157 2.85[53] 0.006[53] 2.17 0.28 0.029 dwarf planet; belt asteroid 1801
Orcus
90482
455+25
−20 		0.0719 0.404 0.0004 0.548±0.010[54] 0.000092 1.4±0.2[54] 0.2 0.0204 plutino; binary 2004
Salacia
120347
423±11 0.0664 0.3729 0.0003 0.492±0.007[55] 0.000082 1.5±0.1[55] 0.165 0.0168 cubewano; binary 2004
2002 MS4
307261
400±12[56] 0.0628 0.2681 0.0002 cubewano 2002
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