The following is a collection of lists of asteroids of the Solar System that are exceptional in some way, such as their size or orbit. For the purposes of this article, "asteroid" refers to minor planets out to the orbit of Neptune, and includes the dwarf planet 1 Ceres, the Jupiter trojans and the centaurs, but not trans-Neptunian objects (objects in the Kuiper belt, scattered disc or inner Oort cloud). For a complete list of minor planets in numerical order, see List of minor planets.
Asteroids are given minor planet numbers, but not all minor planets are asteroids. Minor planet numbers are also given to objects of the Kuiper belt, which is similar to the asteroid belt but farther out (around 30–60 AU), whereas asteroids are mostly between 2–3 AU from the Sun or at the orbit of Jupiter 5 AU from the Sun. Also, comets are not typically included under minor planet numbers, and have their own naming conventions.
Asteroids are given a unique sequential identifying number once their orbit is precisely determined. Prior to this, they are known only by their systematic name or provisional designation, such as .
Estimating the sizes of asteroids from observations is difficult due to their irregular shapes, varying albedo, and small angular diameter. Observations by the Very Large Telescope of most large asteroids were published 2019–2021.[1] [2]
| Name | Picture | Diameter (km) (geometric mean) | Dimensions (km) | Mean distance from Sun (in AU) | Inclination (°) | Date discovered | Discoverer | Class | |
|---|---|---|---|---|---|---|---|---|---|
| 964.4 × 964.2 × 891.8 | 2.766 | 10.6 | G | ||||||
| 572.6 × 557.2 × 446.4 ± 0.2 | 2.362 | 7.14 | V | ||||||
| 568×530×450 | 2.773 | 34.9 | B | ||||||
| 450×430×424 | 3.139 | 5.1 | C | ||||||
| 362×348×310 | 3.062 | 17.3 | F | ||||||
| 378×336×255 | 3.095 | 7.48 | C | ||||||
| 359×293×253 | 3.168 | 15.9 | C | ||||||
| 363×249×191 or 374×248×194 | 3.485 | 10.9 | X | ||||||
| 357×255×212 | 2.643 | 11.75 | S | ||||||
| 294×280×248 | 3.149 | 26.3 | C | ||||||
| 3.439 | 3.56 | C | |||||||
(if bilobe) | 403 × 201 | 5.235 | 18.66 | D | |||||
| 288×250×225 | 2.672 | 12.98 | S | ||||||
| 3.059 | 15.2 | ||||||||
| [3] | 3.476 | 10 | C | ||||||
| 234×224×225 | 2.684 | 11.1 | C | ||||||
| 279×232×189 ± 10% | 2.924 | 3.1 | M | ||||||
| 255×232×193 | 2.769 | 5.22 | B | ||||||
| 257×211×185 | 3.108 | 6.55 | C | ||||||
| 225×205×195 | 2.442 | 1.57 | G | ||||||
| ?[4] | 3.457 | 7.6 | C | ||||||
| 232×220×176 | 3.136 | 0.76 | C | ||||||
| ? (< 200 km) | 225×173 | 3.160 | 7.97 | C | |||||
| 222×209×183 | 2.554 | 6.08 | S | ||||||
| 238×199×182 | 2.576 | 16.54 | G | ||||||
| 262×205×164 | 3.127 | 22.78 | C | ||||||
| 268×234×180[5] | 2.386 | 5.52 | S | ||||||
| 205x185x170 | 2.426 | 14.75 | S | ||||||
| 3.126 | 15.94 | C | |||||||
| 3.195 | 20.59 | C/B | |||||||
| 252×191×138 | 2.720 | 6.61 | F | ||||||
| 235×183×153 | 2.765 | 15.77 | C | ||||||
| 3.065 | 11.23 | C | |||||||
| 3.135 | 10.81 | C/P/X | |||||||
| 3.149 | 23.83 | B | |||||||
| 222×182×130 | 2.385 | 5.58 | S | ||||||
| 2.772 | 16.31 | S | |||||||
| 191×162×144 | 2.798 | 18.4 | S | ||||||
| 178×163×147 | 2.751 | 6.25 | Watson, J. C. | C | |||||
| (4:1 resonance) [sort by 'Mean Distance from Sun' to place in table] | 2.06 | (defines inner edge of main belt) | |||||||
| (3:1 resonance) | 2.50 | (separates inner from middle belt) | |||||||
| (5:2 resonance) | 2.82 | (separates middle from outer belt) | |||||||
| (7:3 resonance) | 2.95 | ||||||||
| (2:1 resonance) | 3.27 | (defines outermost belt) | |||||||
| (1:1 resonance) | 5.20 | (Trojan asteroids - defines outer edge of main belt) | |||||||
The number of bodies grows rapidly as the size decreases. Based on IRAS data there are about 140 main-belt asteroids with a diameter greater than 120 km, which is approximately the transition point between surviving primordial asteroids and fragments thereof.[6] [7] For a more complete list, see List of Solar System objects by size.
The inner asteroid belt (defined as the region interior to the 3:1 Kirkwood gap at 2.50 AU) has few large asteroids. Of those in the above list, only 4 Vesta, 19 Fortuna, 6 Hebe, 7 Iris and 9 Metis orbit there. (Sort table by mean distance.)
Below are the sixteen most-massive measured asteroids.[8] Ceres, at a third the estimated mass of the asteroid belt, is half again as massive as the next fifteen put together. The masses of asteroids are estimated from perturbations they induce on the orbits of other asteroids, except for asteroids that have been visited by spacecraft or have an observable moon, where a direct mass calculation is possible. Different sets of astrometric observations lead to different mass determinations; the biggest problem is accounting for the aggregate perturbations caused by all of the smaller asteroids.[9]
| 938.35 | 0.001% (938.34–938.36) | 39.2% | ||
| 259.076 | 0.0004% (259.075–259.077) | 10.8% | ||
| 204 | 1.5% (201–207) | 8.5% | ||
| 87 | 8% (80–94) | 3.6% | ||
| 35 | 14% (30–40) | 1.5% | ||
| 30 | 6% (29–32) | 1.3% | ||
| 27 | 9% (25–29) | 1.1% | ||
| 27 | 27% (19–34) | 1.1% | ||
| 24 | 16% (20–28) | 1.0% | ||
| 23 | 13% (20–26) | 1.0% | ||
| ≈ 23 | ? | ≈ 1% | ||
| 17 | 18% (14–19) | 0.7% | ||
| 15 | 12% (13 - 17) | 0.6% | ||
| 14.76 | 0.4% (14.70–14.82)[10] | 0.6% | ||
| 14 | 17% (11–16) | 0.6% | ||
| 13 | 16% (11–15) | 0.5% | ||
| 12 | 20% (10–15) | 0.5% | ||
| 12 | 20% (9–14) | 0.5% | ||
| 11.2 | 1% (11.1–11.3)[11] | 0.5% | ||
| 10 | 9% (9–11) | 0.4% | ||
| Total | 1781 | NA | 75% |
|---|
Outside the top four, the ranking of all the asteroids is uncertain, as there is a great deal of overlap among the estimates.
The largest asteroids with an accurately measured mass, because they have been studied by the probe Dawn, are 1 Ceres with a mass of, and 4 Vesta at . The third-largest asteroid with an accurately measured mass, because it has moons, is 87 Sylvia at . Other large asteroids with masses measured from their moons are 107 Camilla and 130 Elektra.[12] [13] [1]
For a more complete list, see List of Solar System objects by size. Other large asteroids such as 423 Diotima currently only have estimated masses.[14] [15]
Only Vesta is regularly bright enough to be seen with the naked eye. Under ideal viewing conditions with very dark skies, a keen eye might be able to also see Ceres, as well as Pallas and Iris at their rare perihelic oppositions.[16] The following asteroids can all reach an apparent magnitude brighter than or equal to the +8.3 attained by Saturn's moon Titan at its brightest, which was discovered 145 years before the first asteroid was found owing to its closeness to the easily observed Saturn.
None of the asteroids in the outer part of the asteroid belt can ever attain this brightness. Even Hygiea and Interamnia rarely reach magnitudes of above 10.0. This is due to the different distributions of spectral types within different sections of the asteroid belt: the highest-albedo asteroids are all concentrated closer to the orbit of Mars, and much lower albedo C and D types are common in the outer belt.
Those asteroids with very high eccentricities will only reach their maximum magnitude rarely, when their perihelion is very close to a heliocentric conjunction with Earth, or (in the case of 99942 Apophis,,, and 367943 Duende) when the asteroid passes very close to Earth.
| Asteroid | Magnitude when brightest | Semi- major axis (AU) | Diameter (km) | Year of discovery | ||
|---|---|---|---|---|---|---|
| 3.4* | 0.922 | 0.191 | 0.32 | 2004 | ||
| 5.20 | 2.361 | 0.089172 | 529 | 1807 | ||
| 6.49 | 2.773 | 0.230725 | 544 | 1802 | ||
| 6.65 | 2.766 | 0.079905 | 952 | 1801 | ||
| 6.73 | 2.385 | 0.231422 | 200 | 1847 | ||
| 6.8 | 1.458 | 0.222725 | 34 × 11 × 11 | 1898 | ||
| 6.85 | 1.711 | 0.467207 | 0.93 | 2001 | ||
| 7.04 | 0.910 | 0.089319 | 0.04 × 0.02 | 2012 | ||
| 7.5 | 2.425 | 0.201726 | 186 | 1847 | ||
| 7.5 | 2.668 | 0.258194 | 233 | 1804 | ||
| 7.5 | 2.296 | 0.218708 | 141 | 1852 | ||
| 7.74 | 1.448 | 0.639770 | 0.5 | 1998 | ||
| 7.9 | 2.643 | 0.187181 | 268 | 1851 | ||
| 7.9 | 2.202 | 0.156207 | 128 | 1847 | ||
| 8.0 | 2.682 | 0.338252 | 229 | 1892 | ||
| 8.1 | 2.6657 | 0.533710 | 32 | 1924 | ||
| 8.1 | 2.387 | 0.121441 | 190 | 1848 | ||
| 8.2 | 2.404 | 0.246216 | 103 | 1879 | ||
| 8.3 | 2.409 | 0.142880 | 145 | 1852 |
* Apophis will only achieve that brightness on April 13, 2029.[17] [18] It typically has an apparent magnitude of 20–22.
See main article: List of slow rotators (minor planets).
This list contains the slowest-rotating known minor planets with a period of at least 1000 hours, or 41 days, while most bodies have rotation periods between 2 and 20 hours. Also see Potentially slow rotators for minor planets with an insufficiently accurate period .
| width=28 | width=180 | Minor planet designation | Rotation period (hours) | Δmag | Quality (U) | Orbit or family | Spectral type | Diameter (km) | Abs. mag (H) | width=100 | Refs | ||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| align=left | 1880 | 0.6 | 2 | align=left | align=right | 0.782 | 17.9 | ||||||
| align=left | 1641 | 0.30 | 2 | align=left | CBU: | align=right | 52.41 | 10.26 | |||||
| align=left | 1561 | 0.80 | 2 | align=left | align=right | 6.51 | 13.1 | ||||||
| align=left | 1332 | 0.18 | 3− | align=left | align=right | 82.14 | 9.30 | ||||||
| align=left | 1320 | 1.34 | 3− | align=left | align=right | 4.62 | 13.60 | ||||||
| align=left | 1265 | 1.40 | 3 | align=left | Hungaria | CX: | align=right | 5.04 | 13.10 | ||||
| align=left | 1256 | 0.42 | 2 | align=left | align=right | 3.40 | 14.65 | ||||||
| align=left | 1234.2 | 0.69 | 2 | align=left | S | align=right | 2.96 | 15.01 | |||||
| align=left | 1170 | 0.90 | 3 | align=left | S | align=right | 32.24 | 10.00 | |||||
| align=left | 1167.4 | 0.80 | 2 | align=left | MBA | align=right | 5.34 | 15.09 | |||||
| align=left | 1072 | 1.25 | 3 | align=left | align=right | 15.47 | 11.61 | ||||||
| align=left | 1069 | 1.26 | 2 | align=left | align=right | 7.14 | 12.90 | ||||||
| align=left | 1060 | 0.75 | 2+ | align=left | Flora | S | align=right | 9.85 | 12.20 | ||||
| align=left | 1007.7 | 0.86 | 2 | align=left | S | align=right | 1.54 | 16.43 |
See main article: List of fast rotators (minor planets).
This list contains the fastest-rotating minor planets with a period of less than 100 seconds, or 0.0277 hours. Bodies with a highly uncertain period, having a quality of less than 2, are highlighted in dark-grey. The fastest rotating bodies are all unnumbered near-Earth objects (NEOs) with a diameter of less than 100 meters (see table).
Among the numbered minor planets with an unambiguous period solution are, a 60-meter sized stony NEO with a period of 352 seconds, as well as and, two main-belt asteroids, with a diameter of 0.86 and 2.25 kilometers and a period of 1.29 and 1.95 hours, respectively (see full list).
| Minor planet designation | Rotation period | Δmag | Quality (U) | Orbit or family | Spectral type | Diameter (km) | Abs. mag (H) | Refs | ||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (seconds) | (hours) | |||||||||||||||
| align=left | 16 | align=left | 0.10 | n.a. | align=left | align=right | 0.012 | 26.80 | align=left | |||||||
| align=left | 18 | align=left | 0.74 | 2 | align=left | NEO | S | align=right | 0.009 | 27.70 | align=left | |||||
| align=left | 25 | align=left | 0.52 | 3 | align=left | NEO | S | align=right | 0.013 | 26.80 | align=left | |||||
| align=left | 30 | align=left | 0.30 | 2 | align=left | NEO | S | align=right | 0.045 | 24.10 | align=left | |||||
| align=left | 31 | align=left | 0.22 | 3 | align=left | NEO | S | align=right | 0.003 | 30.00 | align=left | |||||
| align=left | 31 | align=left | 1.30 | 3 | align=left | NEO | S | align=right | 0.007 | 28.20 | align=left | |||||
| align=left | 34 | align=left | 0.13 | 2 | align=left | NEO | S | align=right | 0.014 | 26.60 | align=left | |||||
| align=left | 43 | align=left | 0.80 | 3− | align=left | NEO | S | align=right | 0.021 | 25.80 | align=left | |||||
| align=left | 43 | align=left | – | n.a. | align=left | NEO | S | align=right | 0.006 | 28.40 | align=left | |||||
| align=left | 46 | align=left | 0.20 | 2− | align=left | NEO | S | align=right | 0.025 | 25.40 | align=left | |||||
| align=left | 52 | align=left | – | n.a. | align=left | NEO | S | align=right | 0.01 | 27.40 | align=left | |||||
| align=left | 57 | align=left | 0.80 | 3 | align=left | NEO | S | align=right | 0.02 | 25.90 | align=left | |||||
| align=left | 66 | align=left | 0.06 | 1 | align=left | NEO | S | align=right | 0.075 | 23.00 | align=left | |||||
| align=left | 70 | align=left | 1.10 | 3 | align=left | NEO | S | align=right | 0.049 | 23.90 | align=left | |||||
| align=left | 70 | align=left | – | n.a. | align=left | NEO | S | align=right | 0.075 | 23.00 | align=left | |||||
| align=left | 77 | align=left | 0.38 | 3− | align=left | NEO | align=right | 0.027 | 25.20 | align=left | ||||||
| align=left | 78 | align=left | 1.39 | 3 | align=left | NEO | S | align=right | 0.037 | 24.54 | align=left | |||||
| align=left | 78 | align=left | 0.08 | 2− | align=left | NEO | S | align=right | 0.011 | 27.10 | align=left | |||||
| align=left | 79 | align=left | 0.32 | 2 | align=left | NEO | S | align=right | 0.039 | 24.40 | align=left | |||||
| align=left | 80 | align=left | 0.66 | 3− | align=left | NEO | S | align=right | 0.094 | 22.50 | align=left | |||||
| align=left | 82 | align=left | – | n.a. | align=left | NEO | S | align=right | 0.012 | 27.00 | align=left | |||||
| align=left | 83 | align=left | 0.92 | 3 | align=left | NEO | S | align=right | 0.005 | 28.90 | align=left | |||||
| align=left | 83 | align=left | – | n.a. | align=left | NEO | S | align=right | 0.022 | 25.70 | align=left | |||||
| align=left | 84 | align=left | 0.66 | 2+ | align=left | NEO | S | align=right | 0.011 | 27.20 | align=left | |||||
| align=left | 86 | align=left | 0.46 | 2+ | align=left | NEO | S | align=right | 0.033 | 24.80 | align=left | |||||
| align=left | 90 | align=left | 0.15 | 2 | align=left | NEO | S | align=right | 0.062 | 23.40 | align=left | |||||
| align=left | 93 | align=left | 0.24 | 2 | align=left | NEO | S | align=right | 0.016 | 26.40 | align=left | |||||
| align=left | 96 | align=left | 0.50 | 3 | align=left | NEO | S | align=right | 0.075 | 23.00 | align=left | |||||
| align=left | 96 | align=left | 0.28 | 2 | align=left | NEO | S | align=right | 0.026 | 25.30 | align=left | |||||
| align=left | 96 | align=left | 0.18 | 2+ | align=left | NEO | S | align=right | 0.007 | 28.30 | align=left | |||||
| align=left | 96 | align=left | 0.53 | 3− | align=left | NEO | S | align=right | 0.018 | 26.10 | align=left | |||||
| align=left | 97 | align=left | 1.02 | 3 | align=left | NEO | align=right | 0.004 | 30.90 | align=left | ||||||
Minor planets with orbital inclinations greater than 90° (the greatest possible is 180°) orbit in a retrograde direction., of the near-800,000 minor planets known, there are only 99 known retrograde minor planets (0.01% of total minor planets known).[19] In comparison, there are over 2,000 comets with retrograde orbits. This makes retrograde minor planets the rarest group of all. High-inclination asteroids are either Mars-crossers (possibly in the process of being ejected from the Solar System) or damocloids. Some of these are temporarily captured in retrograde resonance with the gas giants.[20]
| Minor planet designation | Inclination (°) | width=120pt | First observed/ Discovery date | Condition code | Obs. × arc | Comment | Refs | |
|---|---|---|---|---|---|---|---|---|
| October 27, 2017 | align=center | 0 | 79254 | — | ||||
| September 21, 2018 | align=center | 17407 | — | |||||
| October 8, 2015 | align=center | 0 | 38805 | — | ||||
| September 30, 2005 | align=center | 1 | 12200 | Has a well-determined orbit | ||||
| June 29, 2014 | align=center | 6 | 96 | — | ||||
| March 8, 2010 | align=center | 15 | — | |||||
| September 13, 2015 | align=center | 0 | 184680 | — | ||||
| July 13, 2016 | align=center | 2 | 6075 | — | ||||
| March 29, 2016 | align=center | 0 | 91561 | — | ||||
| August 5, 2014 | align=center | 1 | 8085 | — | ||||
| January 20, 2015 | align=center | 39 | — | |||||
| July 26, 2017 | align=center | 8720 | — | |||||
| May 9, 2014 | align=center | 0 | 95710 | — | ||||
| April 16, 2013 | align=center | 220 | — | |||||
| January 20, 2013 | align=center | 46716 | Has a semi-major axis of 1254 AU, giving it the third largest semi-major axis of any known minor planet | |||||
| April 14, 2010 | align=center | 0 | 97888 | — | ||||
| 100.482° | June 24, 2011 | align=center | 0 | 364936 | — | |||
| 101.295° | July 6, 2017 | align=center | 1 | 28014 | — | |||
| 101.381° | December 8, 2014 | align=center | 0 | 23544 | — | |||
| 101.828° | January 17, 2013 | align=center | 1400 | — | ||||
| 103.396° | May 31, 2008 | align=center | 1 | 198550 | — | |||
| 105.058° | December 18, 2008 | align=center | 0 | 1608789 | — | |||
| 105.113° | August 14, 2016 | align=center | 0 | 63879 | — | |||
| 105.226° | April 6, 2010 | align=center | 0 | 9072 | — | |||
| 106.883° | December 22, 2012 | align=center | 3 | 6674 | — | |||
| 107.449° | February 27, 2009 | align=center | 1584 | — | ||||
| 108.218° | October 29, 2017 | align=center | 1638 | — | ||||
| 108.328° | November 12, 2007 | align=center | 5 | 2204 | — | |||
| 109.074° | September 20, 2011 | align=center | 3 | 3654 | — | |||
| 110.104° | May 31, 2011 | align=center | 1 | 234828 | — | |||
| 110.226° | October 5, 2005 | align=center | 5 | 1488 | — | |||
| 110.504° | May 21, 2010 | align=center | 71808 | — | ||||
| 112.224° | November 1, 2005 | align=center | 4212 | Semi-major axis of 837AU, but has a somewhat short 81-day observation arc for such a large orbit | ||||
| 113.243° | September 17, 2017 | align=center | 4 | 2160 | — | |||
| 2016 LS | 114.338° | June 27, 2015 | align=center | 0 | 26688 | — | ||
| 118.243° | December 29, 2015 | align=center | 0 | 33454 | — | |||
| 118.797° | July 28, 2010 | align=center | 2 | 3535 | — | |||
| 118.970° | September 4, 2002 | align=center | 0 | 648554 | This outer-planet crosser is a damocloid and SDO. | |||
| 121.179° | August 5, 2010 | align=center | 8 | 120 | — | |||
| 123.886° | June 2, 2010 | align=center | 7 | 935 | — | |||
| 125.356° | June 8, 2013 | align=center | 0 | 238336 | — | |||
| 128.506° | September 29, 2014 | align=center | 4 | 1334 | — | |||
| 129.246° | February 25, 2000 | align=center | 2 | 42408 | A damocloid and SDO. Crosses all the outer planets except Neptune. Came within 0.03 AU of Ceres in 1930.[21] | |||
| 129.820° | February 14, 2016 | align=center | 0 | 23800 | — | |||
| 130.333° | July 5, 2013 | align=center | 0 | 143510 | — | |||
| 130.505° | July 6, 2005 | align=center | 1 | 662673 | — | |||
| 133.437° | September 1, 2006 | align=center | 4 | 750 | Has an orbit with a data arc of 25 days | |||
| 136.049° | December 21, 2012 | align=center | 5 | 1066 | — | |||
| 137.204° | January 2, 2017 | align=center | 3 | 1785 | — | |||
| 137.668° | August 17, 2009 | align=center | 1 | 43990 | — | |||
| 138.330° | October 9, 2016 | align=center | 704 | — | ||||
| 139.682° | December 23, 2016 | align=center | 1 | 50718 | — | |||
| 139.758° | March 4, 2019 | align=center | 576 | — | ||||
| 139.934° | November 27, 2014 | align=center | 0 | 115821 | — | |||
| 140.773° | July 1, 2010 | align=center | 0 | 330022 | Perihelion at 9.4 AU, only has perihelion further out (154-day data arc) | |||
| 141.645° | November 24, 2011 | align=center | 108 | — | ||||
| 143.912° | January 25, 2010 | align=center | 1 | 35032 | — | |||
| 143.914° | January 30, 2010 | align=center | 374596 | Semi-major axis of 408 AU with perihelion at 6.1 AU in April 2012 (1 year data arc) | ||||
| 144.034° | November 1, 2012 | align=center | 0 | 227052 | — | |||
| 144.203° | October 23, 2017 | align=center | 68442 | — | ||||
| 146.262° | February 15, 2010 | align=center | 0 | 129000 | — | |||
| 146.883° | April 18, 2012 | align=center | 0 | 31408 | — | |||
| 147.767° | December 17, 2009 | align=center | 0 | 195734 | — | |||
| 148.419° | November 5, 2016 | align=center | 0 | 108624 | — | |||
| 148.826° | August 16, 2017 | align=center | 1 | 45360 | — | |||
| 150.148° | March 5, 2006 | align=center | 0 | 62310 | q=2.58 AU and period=274 yr | |||
| 151.816° | June 12, 1999 | align=center | 2 | 905838 | A damocloid, Jupiter- and Saturn-crossing minor planet.[22] | |||
| 152.044° | September 19, 2017 | align=center | 7590 | — | ||||
| 152.136° | November 19, 2018 | align=center | 7 | 351 | — | |||
| 152.326° | March 3, 2016 | align=center | 0 | 181965 | — | |||
| 152.438° | February 2, 2017 | align=center | 51500 | — | ||||
| 154.367° | April 29, 2009 | align=center | 0 | 771834 | NEO that sometimes has the highest relative velocity to Earth (79 km/s) of known objects that come within 0.5 AU of Earth. However, the relative velocity at 1 AU from the sun is less than 72 km/s. | |||
| 154.736° | June 6, 2013 | align=center | 0 | 14148 | — | |||
| 154.924° | October 11, 2021 | align=center | 3 | 2510 | Retrograde trans-Neptunian object close to a 3:–2 mean-motion orbital resonance with Neptune. | |||
| 155.842° | March 20, 2015 | align=center | 748 | — | ||||
| 156.376° | March 12, 2010 | align=center | 4 | 2460 | — | |||
| 157.514° | December 9, 2015 | align=center | 2 | 5580 | — | |||
| 158.535° | April 29, 2000 | align=center | 2 | 25960 | — | |||
| 159.092° | December 9, 2015 | align=center | 0 | 21120 | — | |||
| 160.027° | October 9, 2012 | align=center | 3 | 900 | — | |||
| 2019 CR | 160.341° | February 4, 2019 | align=center | 1 | 36993 | — | ||
| 160.428° | June 8, 1999 | align=center | 0 | 256779 | most highly inclined known minor planet from June 8, 1999, to July 13, 2004 | |||
| 160.475° | February 25, 2018 | align=center | 0 | 261726 | — | |||
| 160.735° | May 4, 2017 | align=center | 6844 | — | ||||
| 161.695° | June 23, 2015 | align=center | 0 | 119280 | — | |||
| 163.022° | November 26, 2014 | align=center | 0 | 74898 | A Jupiter co-orbital. First known example of a retrograde co-orbital asteroid with any of the planets. Might have an interstellar origin. | Src | ||
| 164.601° | September 14, 2006 | align=center | 5 | 2849 | — | |||
| 165.311° | January 23, 2006 | align=center | 0 | 207459 | — | |||
| 165.525° | July 13, 2004 | align=center | 23944 | Came within 0.80 AU of Saturn on 2007-Jun-05, most highly inclined known minor planet from 2004/07/13-2005/11/01 | ||||
| 165.558° | November 26, 2013 | align=center | 0 | 186598 | — | |||
| 167.030° | February 28, 2016 | align=center | 26 | — | ||||
| 170.324° | September 30, 2008 | align=center | 0 | 1058616 | — | |||
| 170.569° | October 26, 2014 | align=center | 34 | — | ||||
| 170.764° | February 10, 2014 | align=center | 4 | 1938 | — | |||
| 170.919° | October 5, 2018 | align=center | 7 | 270 | — | |||
| 170.988° | March 11, 2016 | align=center | 0 | 18081 | — | |||
| 172.138° | June 3, 2006 | align=center | 48 | Has a data arc of only 2 days, but has a very high inclination | ||||
| 172.872° | November 1, 2005 | align=center | 0 | 228965 | most highly inclined known minor planet from November 1, 2005, to June 1, 2013 | |||
| 175.095° | June 1, 2013 | align=center | 6 | 1075 | Has the highest inclination of any known minor planet |
the value given when the number of observations is multiplied by the observation arc; larger values are generally better than smaller values depending on residuals.
| width=180 | Minor planet designation | Inclination | width=140 | Discovery date | Comment | Refs |
|---|---|---|---|---|---|---|
| 10.593° | January 1, 1801 | most highly inclined known minor planet from January 1, 1801, to March 28, 1802 | ||||
| 34.841° | March 28, 1802 | most highly inclined known minor planet from March 28, 1802, to October 31, 1920 | ||||
| 42.525° | October 31, 1920 | most highly inclined known minor planet from October 31, 1920, to May 22, 1950 | ||||
| 38.949° | August 30, 1935 | First main-belt asteroid discovered to have an inclination greater than 2 Pallas. Most highly inclined known main-belt asteroid from August 30, 1935, to June 14, 1980 | ||||
| 52.083° | May 22, 1950 | most highly inclined known minor planet from May 22, 1950, to July 4, 1973 | ||||
| 41.436° | June 14, 1980 | Most highly inclined known main-belt asteroid from June 14, 1980, to September 20, 2000 | ||||
| 67.999° | July 4, 1973 | An Apollo asteroid, Mars-crosser and +1 km NEO; most highly inclined known minor planet from 4 July 1973 to 8 August 1999. | ||||
| 45.794° | August 17, 1998 | Most highly inclined known main-belt asteroid from August 17, 1998, to October 19, 1998 | ||||
| 51.998° | October 29, 2000 | First main-belt asteroid discovered and numbered to have an inclination greater than 50°. | ||||
| 72.132° | January 4, 2001 | A Mars-crosser and near-Earth object. | ||||
| 77.904° | December 4, 2002 | A damocloid and SDO. It is almost a Uranus outer-grazer. | ||||
| 70.790° | March 6, 2003 | A Mars-crosser, near-Earth object and Jupiter inner-grazer. | ||||
| 64.281° | October 19, 1998 | Most highly inclined known main-belt asteroid from 1998/10/19-2007/11/01 | ||||
| 70.725° | June 9, 2004 | A Mercury- through Mars-crosser and near-Earth object. | ||||
| 68.659° | November 1, 2007 | Most highly inclined known main-belt asteroid from November 1, 2007, to September 26, 2008 | ||||
| 74.247° | September 26, 2008 | Most highly inclined known main-belt asteroid from September 26, 2008, to March 8, 2010 | ||||
| 91.606° | March 8, 2010 | Most highly inclined known main-belt asteroid (orbit is not well-known) |
See main article: List of asteroid close approaches to Earth.
See also: List of minor planets and comets visited by spacecraft.
| width=140 | Name ! | Diameter (km) | Discovered | Spacecraft | Year(s) | Closest approach (km) | Closest approach (asteroid radii) | Notes | Landmark(s) |
|---|---|---|---|---|---|---|---|---|---|
| 939.4 | Dawn | 2014–present | 0.80 | Dawn took its first "close up" picture of Ceres in December 2014, and entered orbit in March 2015 | First likely dwarf planet visited by a spacecraft, largest asteroid visited by a spacecraft | ||||
| 525.4 | Dawn | 2011–2012 | 0.76 | Dawn broke orbit on 5 September 2012 and headed to Ceres, where it arrived in March 2015 | First "big four" asteroid visited by a spacecraft, largest asteroid visited by a spacecraft at the time | ||||
| 120×100×80 | Rosetta | 2010 | 64.9 | Flyby on 10 July 2010 | Largest asteroid visited by a spacecraft at the time | ||||
| 56×24×21 | Galileo | 1993 | 152 | First asteroid with a moon visited by a spacecraft, largest asteroid visited by spacecraft at the time | |||||
| 66×48×46 | NEAR Shoemaker | 1997 | 49.5 | Flyby | Largest asteroid visited by a spacecraft at the time | ||||
| 13×13×33 | NEAR Shoemaker | 1998–2001 | 0 | 1998 flyby; 2000 orbited (first asteroid studied from orbit); 2001 landing | First asteroid landing, first asteroid orbited by a spacecraft, first near-Earth asteroid (NEA) visited by a spacecraft | ||||
| 18.2×10.5×8.9 | Galileo | 1991 | 262 | Flyby | first asteroid visited by a spacecraft | ||||
| 4.6 | Rosetta | 2008 | 302 | Flyby | First asteroid visited by the ESA | ||||
| 4.5×~2 | Chang'e 2 | 2012 | 0.70 | Flyby[23] | Closest asteroid flyby, first asteroid visited by China | ||||
| 4.0 | Stardust | 2002 | 1230 | Flyby | |||||
| 2.2×0.6 | Deep Space 1 | 1999 | 12.7 | ||||||
| 0.5×0.3×0.2 | Hayabusa | 2005 | 0 | Landed; returned dust samples to Earth | First asteroid with returned samples, smallest asteroid visited by a spacecraft, first asteroid visited by a non-NASA spacecraft | ||||
| 1.0 | Hayabusa2 | 2018–2019 | 0 | Multiple landers/rovers, sample return | First rovers on an asteroid | ||||
| 0.492 | OSIRIS-REx | 2018–2021 | 0 | Sample return | Smallest asteroid orbited, potentially hazardous object | ||||
| 0.492 | DART/LICIACube | 2022 | 3.2 | Impactor/flyby | Moon Dimorphos impacted by DART spacecraft, flown by LICIACube | ||||
| 0.790 | Lucy | 2023 | 1076 | Flyby; first of 8 planned asteroid flybys | Smallest main-belt asteroid visited to date; discovered first contact binary satellite Selam |
See main article: Minor-planet moon.
See main article: Active asteroid.
| width=140 | Name ! | Diameter (km) | width=140 | Discovered ! | Comment |
|---|---|---|---|---|---|
| 939 | January 1, 1801 | First asteroid discovered | |||
| 117 | December 8, 1845 | First asteroid discovered after original four (38 years later) | |||
| 136 | September 19, 1852 | First asteroid named after city | |||
| 202 | June 27, 1857 | First asteroid named after living person | |||
| 261 | May 16, 1866 | First asteroid known to have more than one moon (determined in 2005) | |||
| 80×80 | October 1, 1866 | Double asteroid with two nearly equal components; its double nature was discovered using adaptive optics in 2000 | |||
| 126 | 1867 July 7 | Created in one of the largest asteroid-on-asteroid collisions of the past 100 million years | |||
| 217×94 | April 10, 1880 | Metallic asteroid with "ham-bone" shape and 2 satellites | |||
| 56×24×21 | September 29, 1884 | First asteroid known to have a moon (determined in 1994) | |||
| 1.4 | February 17, 1994 | Moon of 243 Ida, first confirmed satellite of an asteroid | |||
| 127 | October 25, 1888 | Orbits in the asteroid belt's outermost edge in a 3:4 orbital resonance with Jupiter | |||
| 32 | February 20, 1890 | Exceptionally slow rotation period of about 1200 hours (2 months) | |||
| 36 | December 22, 1891 | First asteroid discovered by means of astrophotography rather than visual observation | |||
| 13×13×33 | August 13, 1898 | First near-Earth asteroid discovered and the second largest; first asteroid to be detected by radar; first asteroid orbited and landed upon | |||
| 23.3 | March 3, 1902 | First asteroid named after dog | |||
| 115 | September 3, 1902 | Created in one of the largest asteroid-on-asteroid collisions of the past 100 million years | |||
| 135.5 | February 22, 1906 | First Jupiter trojan discovered | |||
| 370×195 | February 10, 1907 | Largest Jupiter trojan discovered | |||
| 2.4 | October 3, 1911 | Last numbered asteroid to be lost then recovered | |||
| 6.4 | September 7, 1920 | First asteroid named after flower | |||
| 13 | February 20, 1928 | Lowest numbered asteroid with no English Wikipedia entry | |||
| 27 | October 30, 1957 | First asteroid discovery to be credited to an institution rather than a person | |||
| 1.4 | June 27, 1949 | First Mercury crosser discovered | |||
| 97 | April 18, 1972 | Last ~100+ km in diameter asteroid discovered | |||
| 21.3 | August 16, 1971 | First asteroid named after cat | |||
| 5 | October 11, 1983 | First asteroid discovered from space; source of Geminids meteor shower. | |||
| 5 | October 10, 1986 | Unusual Earth-associated orbit | |||
| 4.5×2.4×1.9 | January 4, 1989 | Closely approached Earth on September 29, 2004 | |||
| 1.8×0.8 | August 9, 1989 | First asteroid to be radar-imaged in sufficient detail for 3D modeling[24] | |||
| ~2–4 | June 20, 1990 | First Mars trojan (Lagrangian point) discovered | |||
| 1.3 | September 25, 1990 | First automated discovery of a near-Earth object (NEO) | |||
| 1.1 | February 23, 1950 | Will approach Earth very closely in 2880, collision unlikely (1 in 8,300 or 0.012%) | |||
| 0.3 | October 28, 1937 | Named but not numbered until its recovery in 2003 (65 years later) | |||
| 0.3 | June 19, 2004 | First asteroid to rank greater than one on the Torino Scale (it was ranked at 2, then 4; now down to 0). Previously better known by its provisional designation 2004 MN4. | |||
| 0.23 | December 4, 1997 | First asteroid to rank greater than zero on the impact-risk Torino Scale (it was ranked 1; now at 0) | |||
| 0.030 | June 2, 1998 | Approached within 800,000 km of Earth | |||
| 0.1 | January 9, 2002 | Unusual Earth-associated orbit | |||
| 0.030 | March 15, 2004 | Discovered before it approached within 43,000 km of Earth on March 18, 2004. | |||
| ~0.003 | October 6, 2008 | First Earth-impactor to be spotted before impact (on October 7, 2008) | |||
| ~0.3 | October 2010 | First Earth trojan to be discovered | |||
| ~0.017 | September 1, 2014 | Asteroid with fastest rotation: 16.2 seconds | |||
| 152830 Dinkinesh I Selam | 0.22 | November 1, 2023 | First satellite discovered to be a contact-binary |
| width=180 | Name ! | width=180 | Cometary name ! | Comment |
|---|---|---|---|---|
| 95P/Chiron | First centaur discovered in 1977, later identified to exhibit cometary behaviour. Also one of two minor planets (excluding dwarf planets) known to have a ring system | |||
| 107P/Wilson–Harrington | In 1992, it was realized that asteroid 1979 VA's orbit matched it with the positions of the lost comet Wilson–Harrington (1949 III) | |||
| 133P/Elst–Pizarro | Discovered in 1996 as a comet, but orbitally matched to asteroid | |||
| 174P/Echeclus | Centaur discovered in 2000, comet designation assigned in 2006 | |||
| 176P/LINEAR (LINEAR 52) | Main-belt comet–asteroid discovered to have a coma on November 26, 2005 |
The above table lists only numbered asteroids that are also comets. Note there are several cases where a non-numbered minor planets turned out to be a comet, e.g. C/2001 OG108 (LONEOS), which was provisionally designated .
In earlier times, before the modern numbering and naming rules were in effect, asteroids were sometimes given numbers and names before their orbits were precisely known. And in a few cases duplicate names were given to the same object (with modern use of computers to calculate and compare orbits with old recorded positions, this type of error no longer occurs). This led to a few cases where asteroids had to be renamed.[25]
| width=210 | Minor planet name | Description |
|---|---|---|
| An object discovered March 18, 1892, by Max Wolf with provisional designation "1892 X" was named 330 Adalberta, but was lost and never recovered. In 1982 it was determined that the observations leading to the designation of 1892 X were stars, and the object never existed. The name and number 330 Adalberta was then reused for another asteroid discovered by Max Wolf on February 2, 1910, which had the provisional designation A910 CB. | ||
| 525 Adelaide and 1171 Rusthawelia | The object A904 EB discovered March 14, 1904, by Max Wolf was named 525 Adelaide and was subsequently lost. Later, the object 1930 TA discovered October 3, 1930, by Sylvain Arend was named 1171 Rusthawelia. In those pre-computer days, it was not realized until 1958 that these were one and the same object. The name Rusthawelia was kept (and discovery credited to Arend); the name 525 Adelaide was reused for the object 1908 EKa discovered October 21, 1908, by Joel Hastings Metcalf. | |
| The object 1911 LX discovered April 22, 1911, by H. E. Wood was named 715 Transvaalia. On April 23, 1920, the object 1920 GZ was discovered and named 933 Susi. In 1928 it was realized that these were one and the same object. The name Transvaalia was kept, and the name and number 933 Susi was reused for the object 1927 CH discovered February 10, 1927, by Karl Reinmuth. | ||
| The object A917 CB discovered February 13, 1917, by Max Wolf was named 864 Aase, and the object 1926 XB discovered December 7, 1926, by Karl Reinmuth was named 1078 Mentha. In 1958 it was discovered that these were one and the same object. In 1974, this was resolved by keeping the name 1078 Mentha and reusing the name and number 864 Aase for the object 1921 KE, discovered September 30, 1921, by Karl Reinmuth. | ||
| The object 1928 DC discovered February 24, 1928, by Karl Reinmuth was named 1095 Tulipa, and the object 1938 DO discovered February 20, 1938, by Yrjö Väisälä was named 1449 Virtanen. In 1966 it was discovered that these were one and the same object. The name 1449 Virtanen was kept and the name and number 1095 Tulipa was reused for the object 1926 GS discovered April 14, 1926, by Karl Reinmuth. | ||
| The object 1928 UF discovered October 25, 1928, by Zhang Yuzhe (Y. C. Chang) was named 1125 China, and was later lost. Later, the object was discovered on October 30, 1957, at Purple Mountain Observatory and was initially incorrectly believed to be the rediscovery of the object 1928 UF. The name and number 1125 China were then reused for the object, and 1928 UF remained lost. In 1986, the object was discovered and proved to be the real rediscovery of 1928 UF. This object was given the new number and name 3789 Zhongguo. Note Zhongguo is the Mandarin Chinese word for "China", in pinyin transliteration. | ||
| Asteroid 1317 and 787 Moskva | The object 1914 UQ discovered April 20, 1914, by G. N. Neujmin was named 787 Moskva (and retains that name to this day). The object 1934 FD discovered on March 19, 1934, by C. Jackson was given the sequence number 1317. In 1938, G. N. Neujmin found that asteroid 1317 and 787 Moskva were one and the same object. The sequence number 1317 was later reused for the object 1935 RC discovered on September 1, 1935, by Karl Reinmuth; that object is now known as 1317 Silvretta. |
Asteroids were originally named after female mythological figures. Over time the rules loosened.
First asteroid with non-Classical and non-Latinized name: 64 Angelina (in honor of a research station)
First asteroid with a non-feminine name: 139 Juewa (ambiguous) or 141 Lumen
First asteroid with a non-feminized man's name: 903 Nealley
Lowest-numbered unnamed asteroid :
Many landmark numbers had specially chosen names for asteroids, and there was some debate about whether Pluto should have received number 10000, for example. This list includes some non-asteroids.