List of exceptional asteroids

Short description: None

VLT/SPHERE images of most asteroids > 210 km in diameter to scale. Deconvolved with MISTRAL algorithm. Main-belt asteroids > 200 km that were not imaged are (451) Patientia, (65) Cybele and (107) Camilla. Trojan (624) Hektor may also be in this size range. VLT/SPHERE images of a large number of asteroids 100 to 210 km in diameter, to scale. (10) Hygiea, (31) Euphrosyne and (8) Flora have collisional families; all three are round due to having re-coalesced after being disrupted.

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 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). Asteroids are mostly between 2–3 AU from the Sun or at the orbit of Jupiter, 5 AU from the Sun. 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 1950 DA.

## Contents

* 1 Physical characteristics
* 1.1 Largest by diameter
* 1.2 Most massive
* 1.3 Brightest from Earth
* 1.4 Slowest rotators
* 1.5 Fastest rotators
* 2 Orbital characteristics
* 2.1 Retrograde
* 2.2 Highly inclined
* 2.3 Trojans
* 2.4 Record-setting close approaches to Earth
* 3 Viewed in detail
* 3.1 Spacecraft targets
* 3.2 Surface resolved by telescope or lightcurve
* 3.3 Multiple systems resolved by telescope
* 3.4 Comet-like activity
* 3.5 Disintegration
* 4 Timeline
* 4.1 Landmark asteroids
* 4.2 Numbered minor planets that are also comets
* 4.3 Minor planets that were misnamed and renamed
* 4.4 Landmark names
* 5 Landmark numbers
* 6 See also
* 7 Books
* 8 References
* 9 External links

## Physical characteristics

### Largest by diameter

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

|
|
|
|
|
|
|
|

1 Ceres |  | 939.4±0.2 | 964.4 × 964.2 × 891.8 | 2.766  | 10.6 | 1801 | Piazzi, G. | G
4 Vesta |  | 525.4±0.2 | 572.6 × 557.2 × 446.4 ± 0.2 | 2.362  | 7.14 | 1807 | Olbers, H. W. | V
2 Pallas |  | 511±4[1] | 568×530×450 | 2.773  | 34.9 | 1802 | Olbers, H. W. | B
10 Hygiea |  | 433±8[1] | 450×430×424 | 3.139  | 5.1 | 1849 | de Gasparis, A. | C
704 Interamnia |  | 332±5[1] | 362×348×310 | 3.062  | 17.3 | 1910 | Cerulli, V. | F
52 Europa |  | 319±4[1] | 378×336×255 | 3.095  | 7.48 | 1858 | Goldschmidt, H. | C
511 Davida |  | 298±4[1] | 359×293×253 | 3.168  | 15.9 | 1903 | Dugan, R. S. | C
87 Sylvia |  | 271±5[1] | 363×249×191
or 374×248×194 | 3.485  | 10.9 | 1866 | Pogson, N. R. | X
15 Eunomia |  | 270±3[1] | 357×255×212 | 2.643  | 11.75 | 1851 | de Gasparis, A. | S
31 Euphrosyne |  | 268±4[1] | 294×280×248 | 3.149  | 26.3 | 1854 | Ferguson, J. | C
65 Cybele |  | 263±3 | 297 × 291 × 213 | 3.439  | 3.56 | 1861 | Tempel, E. W. | C
624 Hektor |  | 256±12
(if bilobe) | 403 × 201 | 5.235  | 18.66 | 1907 | Kopff, A. | D
3 Juno |  | 254±2[1] | 288×250×225 | 2.672  | 12.98 | 1804 | Harding, K. L. | S
451 Patientia |  | 254±3 |  | 3.059  | 15.2 | 1899 | Charlois, A. |
107 Camilla |  | 254±12[3] |  | 3.476  | 10 | 1868 | Pogson, N. R. | C
324 Bamberga |  | 227±3[1] | 234×224×225 | 2.684  | 11.1 | 1892 | Palisa, J. | C
16 Psyche |  | 223±3[1] | 279×232×189 ± 10% | 2.924  | 3.1 | 1852 | de Gasparis, A. | M
88 Thisbe |  | 218±3[1] | 255×232×193 | 2.769  | 5.22 | 1866 | Peters, C. H. F. | B
48 Doris |  | 215±3[1] | 257×211×185 | 3.108  | 6.55 | 1857 | Goldschmidt, H. | C
19 Fortuna |  | 211±2[1] | 225×205×195 | 2.442  | 1.57 | 1852 | Hind, J. R. | G
121 Hermione |  | 209±5?[4] |  | 3.457  | 7.6 | 1872 | Watson, J. C. | C
24 Themis |  | 208±3[1] | 232×220×176 | 3.136  | 0.76 | 1853 | de Gasparis, A. | C
94 Aurora |  | 205±4 ? (< 200 km)[1] | 225×173 | 3.160  | 7.97 | 1867 | Watson, J. C. | C
29 Amphitrite |  | 204±2[1] | 222×209×183 | 2.554  | 6.08 | 1854 | Marth, A. | S
13 Egeria |  | 202±3[1] | 238×199×182 | 2.576  | 16.54 | 1850 | de Gasparis, A. | G
130 Elektra |  | 199±2[1] | 262×205×164 | 3.127  | 22.78 | 1873 | C. H. F. Peters | C
7 Iris |  | 199±10[1] | 268×234×180[5] | 2.386  | 5.52 | 1847 | Hind, J. R. | S
6 Hebe |  | 195±3[1] | 205x185x170 | 2.426  | 14.75 | 1847 | Hencke, K. L. | S
375 Ursula |  | 192±4 |  | 3.126  | 15.94 | 1893 | Charlois, A. | C
702 Alauda |  | 191±2 |  | 3.195  | 20.59 | 1910 | Helffrich, J. | C/B
45 Eugenia |  | 188±2[1] | 252×191×138 | 2.720  | 6.61 | 1857 | Goldschmidt, H. | F
41 Daphne |  | 187±13[1] | 235×183×153 | 2.765  | 15.77 | 1856 | Goldschmidt, H. | C
154 Bertha |  | 186±2 |  | 3.195  | 20.972 | 1875 | Henry, P. M. | C
423 Diotima |  | 176±4 |  | 3.065  | 11.23 | 1896 | Charlois, A. | C
259 Aletheia |  | 174±1 |  | 3.135  | 10.81 | 1886 | Peters, C. H. F. | C/P/X
372 Palma |  | 174±3 |  | 3.149  | 23.83 | 1893 | Charlois, A. | B
9 Metis |  | 173±2[1] | 222×182×130 | 2.385  | 5.58 | 1848 | Graham, A. | S
532 Herculina |  | 168±1 |  | 2.772  | 16.31 | 1904 | Wolf, M. | S
354 Eleonora |  | 165±3[1] | 191×162×144 | 2.798  | 18.4 | 1893 | Auguste Charlois | S
128 Nemesis |  | 163±5[1] | 178×163×147 | 2.751  | 6.25 | 1872 | 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,[6] which is approximately the transition point between surviving primordial asteroids and fragments thereof.[7][8] 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.)

###  Most massive

Below are the sixteen most-massive measured asteroids.[9] 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.[10]

<div style="border:solid transparent;position:absolute;width:100px;line-height:0;<div style="border:solid transparent;position:absolute;width:100px;line-height:0;<div style="border:solid transparent;position:absolute;width:100px;line-height:0;<div style="border:solid transparent;position:absolute;width:100px;line-height:0;<div style="border:solid transparent;position:absolute;width:100px;line-height:0;<div style="border:solid transparent;position:absolute;width:100px;line-height:0;<div style="border:solid transparent;position:absolute;width:100px;line-height:0;<div style="border:solid transparent;position:absolute;width:100px;line-height:0;<div style="border:solid transparent;position:absolute;width:100px;line-height:0;<div style="border:solid transparent;position:absolute;width:100px;line-height:0;<div style="border:solid transparent;position:absolute;width:100px;line-height:0;<div style="border:solid transparent;position:absolute;width:100px;line-height:0;

Comparative masses of the asteroids with nominal masses > 20×1018 kg.[11]

Ceres (938%)

Vesta (259%)

Pallas (204%)

Hygiea (87%)

Interamnia (35%)

Eunomia (30%)

Juno (27%)

Davida (27%)

Europa (24%)

Psyche (23%)

Herculina (23%)

other (716%)

Asteroids with nominal mass > 10×1018 kg Name  | Mass
(×1018 kg) | Precision  | Approx.
proportion
of all
asteroids

|
|
|

1 Ceres | 938.35 | 0.001% (938.34–938.36) | 39.2%
4 Vesta | 259.076 | 0.0004% (259.075–259.077) | 10.8%
2 Pallas | 204 | 1.5% (201–207) | 8.5%
10 Hygiea | 87 | 8% (80–94) | 3.6%
704 Interamnia | 35 | 14% (30–40) | 1.5%
15 Eunomia | 30 | 6% (29–32) | 1.3%
3 Juno | 27 | 9% (25–29) | 1.1%
511 Davida | 27 | 27% (19–34) | 1.1%
52 Europa | 24 | 16% (20–28) | 1.0%
16 Psyche | 23 | 13% (20–26) | 1.0%
532 Herculina | ≈ 23 | ? | ≈ 1%
31 Euphrosyne | 17 | 18% (14–19) | 0.7%
65 Cybele | 15 | 12% (13-17) | 0.6%
87 Sylvia | 14.76 | 0.4% (14.70–14.82)[12] | 0.6%
7 Iris | 14 | 17% (11–16) | 0.6%
29 Amphitrite | 13 | 16% (11–15) | 0.5%
6 Hebe | 12 | 20% (10–15) | 0.5%
88 Thisbe | 12 | 20% (9–14) | 0.5%
107 Camilla | 11.2 | 1% (11.1–11.3)[3] | 0.5%
324 Bamberga | 10 | 9% (9–11) | 0.4%
Total  | 1781 | NA | 75%

The proportions assume that the total mass of the asteroid belt is 2.39×1021 kg, or (12.4±1.0)×10−10 M☉.[13]

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 (939.3±0.5)×1018 kg, and 4 Vesta at (259.076±0.001)×1018 kg. The third-largest asteroid with an accurately measured mass, because it has moons, is 87 Sylvia at (14.76±0.06)×1018 kg. Other large asteroids with masses measured from their moons are 107 Camilla and 130 Elektra.[3][14][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.[15][16]

### Brightest from Earth

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.[17] 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 cases of 433 Eros, 99942 Apophis, (152680) 1998 KJ9, (153814) 2001 WN5, and 367943 Duende) when the asteroid passes very close to Earth.

Asteroid  | Magnitude
when
brightest | Semi-
major
axis (AU) | Eccentricity
of orbit | Diameter
(km) | Year of
discovery

|
|
|
|
|

99942 Apophis | 3.4* | 0.922 | 0.191 | 0.32 | 2004
4 Vesta | 5.20 | 2.361 | 0.089172 | 529 | 1807
2 Pallas | 6.49 | 2.773 | 0.230725 | 544 | 1802
1 Ceres | 6.65 | 2.766 | 0.079905 | 952 | 1801
7 Iris | 6.73 | 2.385 | 0.231422 | 200 | 1847
433 Eros | 6.8 | 1.458 | 0.222725 | 34 × 11 × 11 | 1898
(153814) 2001 WN5 | 6.85 | 1.711 | 0.467207 | 0.93 | 2001
367943 Duende | 7.04 | 0.910 | 0.089319 | 0.04 × 0.02 | 2012
6 Hebe | 7.5 | 2.425 | 0.201726 | 186 | 1847
3 Juno | 7.5 | 2.668 | 0.258194 | 233 | 1804
18 Melpomene | 7.5 | 2.296 | 0.218708 | 141 | 1852
(152680) 1998 KJ9 | 7.74 | 1.448 | 0.639770 | 0.5 | 1998
15 Eunomia | 7.9 | 2.643 | 0.187181 | 268 | 1851
8 Flora | 7.9 | 2.202 | 0.156207 | 128 | 1847
324 Bamberga | 8.0 | 2.682 | 0.338252 | 229 | 1892
1036 Ganymed | 8.1 | 2.6657 | 0.533710 | 32 | 1924
9 Metis | 8.1 | 2.387 | 0.121441 | 190 | 1848
192 Nausikaa | 8.2 | 2.404 | 0.246216 | 103 | 1879
20 Massalia | 8.3 | 2.409 | 0.142880 | 145 | 1852

* Apophis will only achieve that brightness on April 13, 2029.[18][19] It typically has an apparent magnitude of 20–22.

### Slowest rotators

For a more comprehensive list, see Astronomy: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​2⁄3 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 (U < 2).

#  | Minor planet designation | Rotation period
(hours)  | Δmag | Quality
(U)  | Orbit or family | Spectral type | Diameter
(km)  | Abs. mag
(H)  | Refs

|
|
|
|
|
|
|
|
|

1. | (162058) 1997 AE12 | 1880 | 0.6 | 2 | NEO | S | 0.782 | 17.9 | LCDB * List
2. | 846 Lipperta | 1641 | 0.30 | 2 | Themis | CBU: | 52.41 | 10.26 | LCDB * List
3. | 2440 Educatio | 1561 | 0.80 | 2 | Flora | S | 6.51 | 13.1 | LCDB * List
4. | 912 Maritima | 1332 | 0.18 | 3− | MBA (outer) | C | 82.14 |  9.30 | LCDB * List
5. | 9165 Raup | 1320 | 1.34 | 3− | Hungaria | S | 4.62 | 13.60 | LCDB * List
6. | 1235 Schorria | 1265 | 1.40 | 3 | Hungaria | CX: | 5.04 | 13.10 | LCDB * List
7. | 50719 Elizabethgriffin | 1256 | 0.42 | 2 | Eunomia | S | 3.40 | 14.65 | LCDB * List
8. | (75482) 1999 XC173 | 1234.2 | 0.69 | 2 | Vestian | S | 2.96 | 15.01 | LCDB * List
9. | 288 Glauke | 1170 | 0.90 | 3 | MBA (outer) | S | 32.24 | 10.00 | LCDB * List
10. | (39546) 1992 DT5 | 1167.4 | 0.80 | 2 | MBA (outer) | C | 5.34 | 15.09 | LCDB * List
11. | 496 Gryphia | 1072 | 1.25 | 3 | Flora | S | 15.47 | 11.61 | LCDB * List
12. | 4524 Barklajdetolli | 1069 | 1.26 | 2 | Flora | S | 7.14 | 12.90 | LCDB * List
13. | 2675 Tolkien | 1060 | 0.75 | 2+ | Flora | S | 9.85 | 12.20 | LCDB * List
14. | (219774) 2001 YY145 | 1007.7 | 0.86 | 2 | MBA (inner) | S | 1.54 | 16.43 | LCDB * List

back to top

### Fastest rotators

For a more comprehensive list, see Astronomy: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 (459872) 2014 EK24, a 60-meter sized stony NEO with a period of 352 seconds, as well as (335433) 2005 UW163 and (60716) 2000 GD65, 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)
1. | 2014 RC | 16 | 0.004389 | 0.10 | n.a. | NEO | S | 0.012 | 26.80 | LCDB * MPC
2. | 2015 SV6 | 18 | 0.00490 | 0.74 | 2 | NEO | S | 0.009 | 27.70 | LCDB * MPC
3. | 2010 JL88 | 25 | 0.0068295 | 0.52 | 3 | NEO | S | 0.013 | 26.80 | LCDB * MPC
4. | 2017 EK | 30 | 0.0083 | 0.30 | 2 | NEO | S | 0.045 | 24.10 | LCDB * MPC
5. | 2010 WA | 31 | 0.0085799 | 0.22 | 3 | NEO | S | 0.003 | 30.00 | LCDB * MPC
6. | 2017 UK8 | 31 | 0.0086309 | 1.30 | 3 | NEO | S | 0.007 | 28.20 | LCDB * MPC
7. | 2016 GE1 | 34 | 0.009438 | 0.13 | 2 | NEO | S | 0.014 | 26.60 | LCDB * MPC
8. | 2008 HJ | 43 | 0.01185 | 0.80 | 3− | NEO | S | 0.021 | 25.80 | LCDB * MPC
9. | 2009 TM8 | 43 | 0.012 | – | n.a. | NEO | S | 0.006 | 28.40 | LCDB * MPC
10. | 2015 SU | 46 | 0.0127 | 0.20 | 2− | NEO | S | 0.025 | 25.40 | LCDB * MPC
11. | 2010 SK13 | 52 | 0.0144 | – | n.a. | NEO | S | 0.01 | 27.40 | LCDB * MPC
12. | 2009 BF2 | 57 | 0.01593 | 0.80 | 3 | NEO | S | 0.02 | 25.90 | LCDB * MPC
13. | 2016 GS2 | 66 | 0.0182725 | 0.06 | 1 | NEO | S | 0.075 | 23.00 | LCDB * MPC
14. | 2010 TG19 | 70 | 0.0193935 | 1.10 | 3 | NEO | S | 0.049 | 23.90 | LCDB * MPC
15. | 2008 WA14 | 70 | 0.0195 | – | n.a. | NEO | S | 0.075 | 23.00 | LCDB * MPC
16. | 2007 KE4 | 77 | 0.021408 | 0.38 | 3− | NEO | S | 0.027 | 25.20 | LCDB * MPC
17. | 2000 DO8 | 78 | 0.0217 | 1.39 | 3 | NEO | S | 0.037 | 24.54 | LCDB * MPC
18. | 2014 GQ17 | 78 | 0.0217 | 0.08 | 2− | NEO | S | 0.011 | 27.10 | LCDB * MPC
19. | 2014 TV | 79 | 0.02190 | 0.32 | 2 | NEO | S | 0.039 | 24.40 | LCDB * MPC
20. | 2000 WH10 | 80 | 0.02221 | 0.66 | 3− | NEO | S | 0.094 | 22.50 | LCDB * MPC
21. | 2012 HG2 | 82 | 0.0227 | – | n.a. | NEO | S | 0.012 | 27.00 | LCDB * MPC
22. | 2010 TD54 | 83 | 0.0229317 | 0.92 | 3 | NEO | S | 0.005 | 28.90 | LCDB * MPC
23. | 2010 TS19 | 83 | 0.023 | – | n.a. | NEO | S | 0.022 | 25.70 | LCDB * MPC
24. | 2009 UD | 84 | 0.023246 | 0.66 | 2+ | NEO | S | 0.011 | 27.20 | LCDB * MPC
25. | 2014 WB366 | 86 | 0.0238 | 0.46 | 2+ | NEO | S | 0.033 | 24.80 | LCDB * MPC
26. | 2015 RF36 | 90 | 0.025 | 0.15 | 2 | NEO | S | 0.062 | 23.40 | LCDB * MPC
27. | 2015 AK45 | 93 | 0.0258 | 0.24 | 2 | NEO | S | 0.016 | 26.40 | LCDB * MPC
28. | 2010 XE11 | 96 | 0.0265846 | 0.50 | 3 | NEO | S | 0.075 | 23.00 | LCDB * MPC
29. | 2000 UK11 | 96 | 0.026599 | 0.28 | 2 | NEO | S | 0.026 | 25.30 | LCDB * MPC
30. | 2016 RB1 | 96 | 0.02674 | 0.18 | 2+ | NEO | S | 0.007 | 28.30 | LCDB * MPC
31. | 2015 CM | 96 | 0.0268 | 0.53 | 3− | NEO | S | 0.018 | 26.10 | LCDB * MPC
32. | 2008 TC3 | 97 | 0.0269409 | 1.02 | 3 | NEO | F | 0.004 | 30.90 | LCDB * MPC

back to top

## Orbital characteristics

### Retrograde

Minor planets with orbital inclinations near or greater than 90° (the greatest possible is 180°) orbit in a retrograde direction. As of March 2018[update], of the near-800,000 minor planets known, there are only 99 known retrograde minor planets (0.01% of total minor planets known).[20] 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.[21]

Minor planet
designation | Inclination (°)  | First observed/
Discovery date  | Condition code  | Obs. × arc[2] | Comment  | Refs

|
|
|
|
|
|

2024 TF3 | 89.1°  | March 8, 2010  |  | 40  | MPC
2017 UX51 | 090.517 90.5°  | October 27, 2017 | 0 | 79254 | — | MPC
2018 SQ13 | 090.973 90.9°  | September 21, 2018 | 9  | 17407 | — | MPC
2015 TN178 | 091.093 91.0°  | October 8, 2015 | 0 | 38805 | — | MPC
2005 SB223 | 091.294 91.2°  | September 30, 2005 | 1 | 12200 | Has a well-determined orbit | MPC
2014 MH55 | 091.486 91.4°  | June 29, 2014 | 6 | 96 | — | MPC
2010 EQ169 | 091.607 91.6°  | March 8, 2010 | 9 ?  | 15 | Most highly inclined known main-belt asteroid (orbit is not well-known) | MPC
2015 RK245 | 091.616 91.6°  | September 13, 2015 | 0 | 184680 | — | MPC
2016 TK2 | 092.336 92.3°  | July 13, 2016 | 2 | 6075 | — | MPC
(518151) 2016 FH13 | 093.551 93.5°  | March 29, 2016 | 0 | 91561 | — | MPC
2014 PP69 | 093.652 93.6°  | August 5, 2014 | 1 | 8085 | — | MPC
2015 BH311 | 094.160 94.1°  | January 20, 2015 | 9 ?  | 39 | — | MPC
2017 OX68 | 094.748 94.7°  | July 26, 2017 | 9  | 8720 | — | MPC
2014 JJ57 | 095.924 95.9°  | May 9, 2014 | 0 | 95710 | — | MPC
2013 HS150 | 097.434 97.4°  | April 16, 2013 | 9  | 220 | — | MPC
(709487) 2013 BL76 | 098.592 98.5°  | January 20, 2013 | 9  | 46716 | Has a semi-major axis of 1254 AU, giving it the third largest semi-major axis of any known minor planet | MPC
2010 GW147 | 099.835 99.8°  | April 14, 2010 | 0 | 97888 | — | MPC
2011 MM4 | 100.4° | June 24, 2011 | 0 | 364936 | — | MPC
2017 NM2 | 101.2° | July 6, 2017 | 1 | 28014 | — | MPC
2014 XS3 | 101.3° | December 8, 2014 | 0 | 23544 | — | MPC
2013 BN27 | 101.8° | January 17, 2013 | 9  | 1400 | — | MPC
(528219) 2008 KV42 | 103.3° | May 31, 2008 | 1 | 198550 | — | MPC
(342842) 2008 YB3 | 105.0° | December 18, 2008 | 0 | 1608789 | — | MPC
2016 PN66 | 105.1° | August 14, 2016 | 0 | 63879 | — | MPC
2010 GW64 | 105.2° | April 6, 2010 | 0 | 9072 | — | MPC
2012 YO6 | 106.8° | December 22, 2012 | 3 | 6674 | — | MPC
2009 DD47 | 107.4° | February 27, 2009 | 9 ?  | 1584 | — | MPC
2017 UR52 | 108.2° | October 29, 2017 | 9  | 1638 | — | MPC
2007 VW266 | 108.3° | November 12, 2007 | 5 | 2204 | — | MPC
2011 SP25 | 109.0° | September 20, 2011 | 3 | 3654 | — | MPC
471325 Taowu | 110.1° | May 31, 2011 | 1 | 234828 | — | MPC
2005 TJ50 | 110.2° | October 5, 2005 | 5 | 1488 | — | MPC
2011 OR17 | 110.5° | May 21, 2010 | 9  | 71808 | — | MPC
2005 VX3 | 112.2° | November 1, 2005 | 9  | 4212 | Semi-major axis of 837AU, but has a somewhat short 81-day observation arc for such a large orbit | MPC
2017 SV13 | 113.2° | September 17, 2017 | 4 | 2160 | — | MPC
2016 LS | 114.3° | June 27, 2015 | 0 | 26688 | — | MPC
2015 YY18 | 118.2° | December 29, 2015 | 0 | 33454 | — | MPC
2010 OM101 | 118.7° | July 28, 2010 | 2 | 3535 | — | MPC
(65407) 2002 RP120 | 118.9° | September 4, 2002 | 0 | 648554 | This outer-planet crosser is a damocloid and SDO. | MPC
2010 PO58 | 121.1° | August 5, 2010 | 8 | 120 | — | MPC
2010 LG61 | 123.8° | June 2, 2010 | 7 | 935 | — | MPC
(468861) 2013 LU28 | 125.3° | June 8, 2013 | 0 | 238336 | — | MPC
2014 SQ339 | 128.5° | September 29, 2014 | 4 | 1334 | — | MPC
2000 DG8 | 129.2° | February 25, 2000 | 2 | 42408 | A damocloid and SDO. Crosses all the outer planets except Neptune. Came within 0.03 AU of Ceres in 1930.[22] | MPC
2016 CO264 | 129.8° | February 14, 2016 | 0 | 23800 | — | MPC
2013 NS11 | 130.3° | July 5, 2013 | 0 | 143510 | — | MPC
2005 NP82 | 130.5° | July 6, 2005 | 1 | 662673 | — | MPC
2006 RG1 | 133.4° | September 1, 2006 | 4 | 750 | Has an orbit with a data arc of 25 days | MPC
2012 YE8 | 136.0° | December 21, 2012 | 5 | 1066 | — | MPC
2017 AX13 | 137.2° | January 2, 2017 | 3 | 1785 | — | MPC
2009 QY6 | 137.6° | August 17, 2009 | 1 | 43990 | — | MPC
2016 TP93 | 138.3° | October 9, 2016 | 9 ?  | 704 | — | MPC
2016 YB13 | 139.6° | December 23, 2016 | 1 | 50718 | — | MPC
2019 EJ3 | 139.7° | March 4, 2019 | 9 ?  | 576 | — | MPC
2015 AO44 | 139.9° | November 27, 2014 | 0 | 115821 | — | MPC
(336756) 2010 NV1 | 140.7° | July 1, 2010 | 0 | 330022 | Perihelion at 9.4 AU, only 2008 KV42 has perihelion further out (154-day data arc) | MPC
2011 WS41 | 141.6° | November 24, 2011 | 9 ?  | 108 | — | MPC
2010 OR1 | 143.9° | January 25, 2010 | 1 | 35032 | — | MPC
2010 BK118 | 143.9° | January 30, 2010 | 9  | 374596 | Semi-major axis of 408 AU with perihelion at 6.1 AU in April 2012 (1 year data arc) | MPC
(523797) 2016 NM56 | 144.0° | November 1, 2012 | 0 | 227052 | — | MPC
2017 UW51 | 144.2° | October 23, 2017 | 9  | 68442 | — | MPC
2010 CG55 | 146.2° | February 15, 2010 | 0 | 129000 | — | MPC
2012 HD2 | 146.8° | April 18, 2012 | 0 | 31408 | — | MPC
2009 YS6 | 147.7° | December 17, 2009 | 0 | 195734 | — | MPC
2016 VY17 | 148.4° | November 5, 2016 | 0 | 108624 | — | MPC
2017 QO33 | 148.8° | August 16, 2017 | 1 | 45360 | — | MPC
2006 EX52 | 150.1° | March 5, 2006 | 0 | 62310 | q=2.58 AU and period=274 yr | MPC
(612093) 1999 LE31 | 151.8° | June 12, 1999 | 2 | 905838 | A damocloid, Jupiter- and Saturn-crossing minor planet.[23] | MPC
2017 SN33 | 152.0° | September 19, 2017 | 9  | 7590 | — | MPC
2018 WB1 | 152.1° | November 19, 2018 | 7 | 351 | — | MPC
2016 JK24 | 152.3° | March 3, 2016 | 0 | 181965 | — | MPC
2017 CW32 | 152.4° | February 2, 2017 | 9  | 51500 | — | MPC
343158 Marsyas | 154.3° | April 29, 2009 | 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. | MPC
2013 LD16 | 154.7° | June 6, 2013 | 0 | 14148 | — | MPC
2021 TH165 | 154.9° | October 11, 2021 | 3 | 2510 | Retrograde trans-Neptunian object close to a 3:–2 mean-motion orbital resonance with Neptune. | MPC
2015 FK37 | 155.8° | March 20, 2015 | 9 ?  | 748 | — | MPC
2010 EB46 | 156.3° | March 12, 2010 | 4 | 2460 | — | MPC
2015 XR384 | 157.5° | December 9, 2015 | 2 | 5580 | — | MPC
2000 HE46 | 158.5° | April 29, 2000 | 2 | 25960 | — | MPC
2015 XX351 | 159.0° | December 9, 2015 | 0 | 21120 | — | MPC
2012 TL139 | 160.0° | October 9, 2012 | 3 | 900 | — | MPC
2019 CR | 160.3° | February 4, 2019 | 1 | 36993 | — | MPC
20461 Dioretsa | 160.4° | June 8, 1999 | 0 | 256779 | most highly inclined known minor planet from June 8, 1999, to July 13, 2004 | MPC
2018 DO4 | 160.4° | February 25, 2018 | 0 | 261726 | — | MPC
2017 JB6 | 160.7° | May 4, 2017 | 9 ?  | 6844 | — | MPC
(523800) 2017 KZ31 | 161.6° | June 23, 2015 | 0 | 119280 | — | MPC
514107 Kaʻepaokaʻāwela | 163.0° | November 26, 2014 | 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. | MPC
Src
2006 RJ2 | 164.6° | September 14, 2006 | 5 | 2849 | — | MPC
2006 BZ8 | 165.3° | January 23, 2006 | 0 | 207459 | — | MPC
2004 NN8 | 165.5° | July 13, 2004 | 9  | 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 | MPC
(459870) 2014 AT28 | 165.5° | November 26, 2013 | 0 | 186598 | — | MPC
2016 DF2 | 167.0° | February 28, 2016 | 9 ?  | 26 | — | MPC
(330759) 2008 SO218 | 170.3° | September 30, 2008 | 0 | 1058616 | — | MPC
2014 UV114 | 170.5° | October 26, 2014 | 9 ?  | 34 | — | MPC
2014 CW14 | 170.7° | February 10, 2014 | 4 | 1938 | — | MPC
2018 TL6 | 170.9° | October 5, 2018 | 7 | 270 | — | MPC
2016 EJ203 | 170.9° | March 11, 2016 | 0 | 18081 | — | MPC
2006 LM1 | 172.1° | June 3, 2006 | 9 ?  | 48 | Has a data arc of only 2 days, but has a very high inclination | MPC
(434620) 2005 VD | 172.8° | November 1, 2005 | 0 | 228965 | most highly inclined known minor planet from November 1, 2005, to June 1, 2013 | MPC
2015 FR561 | 174.3° | March 18, 2015 | 9 | 165 | Has a short data arc of 11 days and is now lost, but has a very high inclination. Thought to be Uranus- and Neptune-crossing. | MPC
2013 LA2 | 175.0° | June 1, 2013 | 6 | 1075 | Has the highest inclination of any known minor planet | MPC

^ 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.

###  Highly inclined

Minor planet designation | Inclination | Discovery date  | Comment  | Refs

|
|
|
|

1 Ceres | 10.593°  | January 1, 1801  | most highly inclined known minor planet from January 1, 1801, to March 28, 1802  | MPC
2 Pallas | 34.841°  | March 28, 1802  | most highly inclined known minor planet from March 28, 1802, to October 31, 1920  | MPC
944 Hidalgo | 42.525°  | October 31, 1920  | most highly inclined known minor planet from October 31, 1920, to May 22, 1950  | MPC
1373 Cincinnati | 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  | MPC
1580 Betulia | 52.083°  | May 22, 1950  | most highly inclined known minor planet from May 22, 1950, to July 4, 1973  | MPC
2938 Hopi | 41.436°  | June 14, 1980  | Most highly inclined known main-belt asteroid from June 14, 1980, to September 20, 2000  | MPC
(5496) 1973 NA | 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.  | MPC
(22653) 1998 QW2 | 45.794°  | August 17, 1998  | Most highly inclined known main-belt asteroid from August 17, 1998, to October 19, 1998  | MPC
(88043) 2000 UE110 | 51.998°  | October 29, 2000  | First main-belt asteroid discovered and numbered to have an inclination greater than 50°.  | MPC
(138925) 2001 AU43 | 72.132°  | January 4, 2001  | A Mars-crosser and near-Earth object.  | MPC
(127546) 2002 XU93 | 77.904°  | December 4, 2002  | A damocloid and SDO. It is almost a Uranus outer-grazer.  | MPC
(196256) 2003 EH1 | 70.790°  | March 6, 2003  | A Mars-crosser, near-Earth object and Jupiter inner-grazer.  | MPC
1998 UQ1 | 64.281°  | October 19, 1998  | Most highly inclined known main-belt asteroid from 1998/10/19-2007/11/01  | MPC
(467372) 2004 LG | 70.725°  | June 9, 2004  | A Mercury- through Mars-crosser and near-Earth object.  | MPC
2007 VR6 | 68.659°  | November 1, 2007  | Most highly inclined known main-belt asteroid from November 1, 2007, to September 26, 2008  | MPC
2008 SB85 | 74.247°  | September 26, 2008  | MPC

### Trojans

* Earth trojans: (706765) 2010 TK7 and (614689) 2020 XL5.
* Mars trojans: (121514) 1999 UJ7, 5261 Eureka, (101429) 1998 VF31, (311999) 2007 NS2, (385250) 2001 DH47, (816688) 2011 SC191, 2011 UN63, and the candidate 2011 SL25.
* Jupiter trojans: the first one was discovered in 1906, 588 Achilles, and the current total is over 15,000.

### Record-setting close approaches to Earth

Main article: Astronomy:List of asteroid close approaches to Earth

## Viewed in detail

### Spacecraft targets

Name | Diameter
(km) | Discovered | Spacecraft | Year(s) | Closest
approach
(km) | Closest
approach
(asteroid radii) | Notes | Landmark(s)

|
|
|
|
|
|
|
|

000001 1 Ceres | 939.4 | 1801 | Dawn | 2014–2018 | 375 | 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
000004 4 Vesta | 525.4 | 1807 | Dawn | 2011–2012 | 210 | 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
000021 21 Lutetia | 120×100×80 | 1852 | Rosetta | 2010 | 3,162 | 64.9 | Flyby on 10 July 2010 | Largest asteroid visited by a spacecraft at the time
000243 243 Ida | 56×24×21 | 1884 | Galileo | 1993 | 2,390 | 152 | Flyby; discovered Dactyl | First asteroid with a moon visited by a spacecraft, largest asteroid visited by spacecraft at the time
000253 253 Mathilde | 66×48×46 | 1885 | NEAR Shoemaker | 1997 | 1,212 | 49.5 | Flyby | Largest asteroid visited by a spacecraft at the time
000433 433 Eros | 13×13×33 | 1898 | NEAR Shoemaker | 1998–2001 | 0 | 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
000951 951 Gaspra | 18.2×10.5×8.9 | 1916 | Galileo | 1991 | 1,600 | 262 | Flyby | First asteroid visited by a spacecraft
002867 2867 Šteins | 4.6 | 1969 | Rosetta | 2008 | 800 | 302 | Flyby | First asteroid visited by the ESA
004179 4179 Toutatis | 4.5×~2 | 1934 | Chang'e 2 | 2012 | 3.2 | 0.70 | Flyby[24] | Closest asteroid flyby, first asteroid visited by China
005535 5535 Annefrank | 4.0 | 1942 | Stardust | 2002 | 3,079 | 1230 | Flyby |
009969 9969 Braille | 2.2×0.6 | 1992 | Deep Space 1 | 1999 | 26 | 12.7 | Flyby; followed by flyby of Comet Borrelly |
025143 25143 Itokawa | 0.5×0.3×0.2 | 1998 | Hayabusa | 2005 | 0 | 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
162173 162173 Ryugu | 1.0 | 1999 | Hayabusa2 | 2018–2019 | 0 | 0 | Multiple landers/rovers, sample return | First rovers on an asteroid
101955 101955 Bennu | 0.492 | 1999 | OSIRIS-REx | 2018–2021 | 0 | 0 | Sample return | Smallest asteroid orbited, potentially hazardous object
65803 65803 Didymos | 0.492 | 1999 | DART/LICIACube | 2022 | 1.2 | 3.2 | Impactor/flyby | Moon Dimorphos impacted by DART spacecraft, flown by LICIACube
152830 152830 Dinkinesh | 0.790 | 1999 | Lucy | 2023 | 425 | 1076 | Flyby; first of 8 planned asteroid flybys | Smallest main-belt asteroid visited to date; discovered first contact binary satellite Selam
52246 52246 Donaldjohanson | 3.9 | 1981 | Lucy | 2025 | 960 | 240 | Flyby; second of 8 planned asteroid flybys |

### Surface resolved by telescope or lightcurve

* 1 Ceres
* 2 Pallas
* 3 Juno
* 4 Vesta
* 5 Astraea
* 6 Hebe
* 7 Iris
* 8 Flora
* 9 Metis
* 10 Hygiea
* 12 Victoria
* 13 Egeria
* 14 Irene
* 15 Eunomia
* 16 Psyche
* 18 Melpomene
* 26 Proserpina
* 29 Amphitrite
* 35 Leukothea
* 37 Fides
* 51 Nemausa
* 52 Europa
* 65 Cybele
* 87 Sylvia
* 89 Julia
* 121 Hermione
* 130 Elektra
* 201 Penelope
* 216 Kleopatra
* 324 Bamberga
* 511 Davida
* 925 Alphonsina
* 1140 Crimea
* 9969 Braille
* (33342) 1998 WT24
* 66391 Moshup
* (136617) 1994 CC
* (285263) 1998 QE2
* (357439) 2004 BL86

### Multiple systems resolved by telescope

Main article: Astronomy:Minor-planet moon

* 90 Antiope

### Comet-like activity

Main article: Astronomy:Active asteroid

* 2006 VW139
* P/2013 P5

### Disintegration

* 6478 Gault
* P/2013 R3

## Timeline

### Landmark asteroids

Name | Diameter (km) | Discovered | Comment

|
|
|

1 Ceres | 939 | January 1, 1801 | First asteroid discovered
5 Astraea | 117 | December 8, 1845 | First asteroid discovered after original four (38 years later)
20 Massalia | 136 | September 19, 1852 | First asteroid named after a city (Marseille)
45 Eugenia | 202 | June 27, 1857 | First asteroid named after living person
87 Sylvia | 261 | May 16, 1866 | First asteroid known to have more than one moon (determined in 2005)
90 Antiope | 80×80 | October 1, 1866 | Double asteroid with two nearly equal components; its double nature was discovered using adaptive optics in 2000
216 Kleopatra | 217×94 | April 10, 1880 | Metallic asteroid with "ham-bone" shape and 2 satellites
243 Ida | 56×24×21 | September 29, 1884 | First asteroid known to have a moon (determined in 1994)
243 Ida I Dactyl | 1.4 | February 17, 1994 | Moon of 243 Ida, first confirmed satellite of an asteroid
279 Thule | 127 | October 25, 1888 | Orbits in the asteroid belt's outermost edge in a 3:4 orbital resonance with Jupiter
288 Glauke | 32 | February 20, 1890 | Exceptionally slow rotation period of about 1200 hours (2 months)
323 Brucia | 36 | December 22, 1891 | First asteroid discovered by means of astrophotography rather than visual observation
433 Eros | 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
482 Petrina | 23.3 | March 3, 1902 | First asteroid named after dog
490 Veritas | 115 | September 3, 1902 | Created in one of the largest asteroid-on-asteroid collisions of the past 100 million years
588 Achilles | 135.5 | February 22, 1906 | First Jupiter trojan discovered
624 Hektor | 370×195 | February 10, 1907 | Largest Jupiter trojan discovered
719 Albert | 2.4 | October 3, 1911 | Last numbered asteroid to be lost then recovered
935 Clivia | 6.4 | September 7, 1920 | First asteroid named after flower
1090 Sumida | 13 | February 20, 1928 | Lowest numbered asteroid with no English Wikipedia entry
1125 China | 27 | October 30, 1957 | First asteroid discovery to be credited to an institution rather than a person
1566 Icarus | 1.4 | June 27, 1949 | First Mercury crosser discovered
2309 Mr. Spock | 21.3 | August 16, 1971 | First asteroid named after cat
3200 Phaethon | 5 | October 11, 1983 | First asteroid discovered from space; source of Geminids meteor shower.
3753 Cruithne | 5 | October 10, 1986 | Unusual Earth-associated orbit
4179 Toutatis | 4.5×2.4×1.9 | January 4, 1989 | Closely approached Earth on September 29, 2004
4769 Castalia | 1.8×0.8 | August 9, 1989 | First asteroid to be radar-imaged in sufficient detail for 3D modeling[25]
5261 Eureka | ~2–4 | June 20, 1990 | First Mars trojan (Lagrangian point L5) discovered
11885 Summanus | 1.3 | September 25, 1990 | First automated discovery of a near-Earth object (NEO)
(29075) 1950 DA | 1.1 | February 23, 1950 | Small chance to collide with Earth in 2880 (1 in 2,600 or 0.039%)[26]
69230 Hermes | 0.3 | October 28, 1937 | Named but not numbered until its recovery in 2003 (65 years later)
99942 Apophis | 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.
152830 Dinkinesh I Selam | 0.22 | November 1, 2023 | First satellite discovered to be a contact-binary
(433953) 1997 XR2 | 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)
1998 KY26 | 0.030 | June 2, 1998 | Approached within 800,000 km of Earth
2002 AA29 | 0.1 | January 9, 2002 | Unusual Earth-associated orbit
2004 FH | 0.030 | March 15, 2004 | Discovered before it approached within 43,000 km of Earth on March 18, 2004.
2008 TC3 | ~0.003 | October 6, 2008 | First Earth-impactor to be spotted before impact (on October 7, 2008)
(706765) 2010 TK7 | ~0.3 | October 2010 | First Earth trojan to be discovered
2014 RC | ~0.017 | September 1, 2014 | Asteroid with fastest rotation: 16.2 seconds

### Numbered minor planets that are also comets

Name | Cometary name | Comment

|
|

2060 Chiron | 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
4015 Wilson–Harrington | 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)
7968 Elst–Pizarro | 133P/Elst–Pizarro | Discovered in 1996 as a comet, but orbitally matched to asteroid 1979 OW7
60558 Echeclus | 174P/Echeclus | Centaur discovered in 2000, comet designation assigned in 2006
118401 LINEAR | 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 2001 OG108.

### Minor planets that were misnamed and renamed

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.[27]

Minor planet name  | Description

|

330 Adalberta | 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.
715 Transvaalia and 933 Susi | 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.
864 Aase and 1078 Mentha | 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.
1095 Tulipa and 1449 Virtanen | 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.
1125 China and 3789 Zhongguo | 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 1957 UN1 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 1957 UN1, and 1928 UF remained lost. In 1986, the object 1986 QK1 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.

### Landmark names

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: 433 Eros

Lowest-numbered unnamed asteroid (As of 2024[update]): (4596) 1981 QB

## Landmark numbers

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.

Template:Flexbox

Template:Flexbox

## See also

* List of minor planets
* List of minor planets named after people
* List of minor planets named after places
* List of instrument-resolved minor planets
* List of minor planet moons
* List of Mercury-crossing minor planets
* List of Venus-crossing minor planets
* List of Earth-crossing asteroids
* List of Mars-crossing minor planets
* List of Jupiter-crossing minor planets
* List of Saturn-crossing minor planets
* List of Uranus-crossing minor planets
* List of Neptune-crossing minor planets
* List of Solar System objects by size
* Lists of astronomical objects
* List of predicted asteroid impacts on Earth
* Small Solar System body
* Amor asteroid
* Apollo asteroid
* Aten asteroid
* Atira asteroid
* Centaur (small Solar System body)
* ʻOumuamua

## Books

* Dictionary of Minor Planet Names, 5th ed.: Prepared on Behalf of Commission 20 Under the Auspices of the International Astronomical Union, Lutz D. Schmadel, ISBN 3-540-00238-3

## References

1. ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 1.11 1.12 1.13 1.14 1.15 1.16 1.17 1.18 1.19 1.20 1.21 1.22 1.23 1.24 1.25 1.26 1.27 P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. Astronomy & Astrophysics 54, A56
2. ↑ As of Jan 2019, good rotational coverage (≥ 4 epochs) had also been obtained for 476 Hedwig and 596 Scheila.[1]
3. ↑ 3.0 3.1 3.2 M. Pajuelo, Benoit Carry, Frédéric Vachier, Michael Marsset et al. (March 2018) Physical, spectral, and dynamical properties of asteroid (107) Camilla and its satellites, Icarus 309
4. ↑ "Small-Body Database Lookup". https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/?sstr=121 Hermione.
5. ↑ Hanuš, J.; Marsset, M.; Vernazza, P.; Viikinkoski, M.; Drouard, A.; Brož, M. et al. (24 April 2019). "The shape of (7) Iris as evidence of an ancient large impact?". Astronomy & Astrophysics 624 (A121): A121. doi:10.1051/0004-6361/201834541. Bibcode: 2018DPS....5040406H.
6. ↑ "JPL Small-Body Database Search Engine: asteroids and orbital class (IMB or MBA or OMB) and diameter > 120 (km)". JPL Solar System Dynamics. http://ssd.jpl.nasa.gov/sbdb_query.cgi?obj_group=all;obj_kind=ast;obj_numbered=all;ast_orbit_class=IMB;ast_orbit_class=MBA;ast_orbit_class=OMB;OBJ_field=0;ORB_field=0;c1_group=OBJ;c1_item=Ap;c1_op=>;c1_value=120;table_format=HTML;max_rows=500;format_option=comp;c_fields=AcApAiBhBgBjBiBnBs;.cgifields=format_option;.cgifields=ast_orbit_class;.cgifields=table_format;.cgifields=obj_kind;.cgifields=obj_group;.cgifields=obj_numbered;.cgifields=com_orbit_class&query=1&c_sort=ApD.
7. ↑ Bottkejr, W; Durda, D; Nesvorny, D; Jedicke, R; Morbidelli, A; Vokrouhlicky, D; Levison, H (May 2005). "The fossilized size distribution of the main asteroid belt" (in en). Icarus 175 (1): 111–140. doi:10.1016/j.icarus.2004.10.026. Bibcode: 2005Icar..175..111B. https://linkinghub.elsevier.com/retrieve/pii/S0019103504003811.
8. ↑ "NASA Astrobiology". https://astrobiology.nasa.gov/news/primordial-asteroids-and-the-stories-they-are-telling/.
9. ↑ "Recent Asteroid Mass Determinations" . Maintained by Jim Baer. Last updated 2010-12-12. Access date 2011-09-02.
10. ↑ Baer, James; Steven R. Chesley (2008). "Astrometric masses of 21 asteroids, and an integrated asteroid ephemeris". Celestial Mechanics and Dynamical Astronomy (Springer Science+Business Media) 100 (2008): 27–42. doi:10.1007/s10569-007-9103-8. Bibcode: 2008CeMDA.100...27B.
11. ↑ assuming a total Main Belt mass of 2394×1018 kg. The mass of Herculina is particularly uncertain
12. ↑ F. Marchis; et al. (2005). "Discovery of the triple asteroidal system 87 Sylvia" (PDF). Nature. 436 (7052): 822–4. Bibcode:2005Natur.436..822M. doi:10.1038/nature04018. PMID 16094362. S2CID 4412813
13. ↑ Pitjeva, E. V. (May 2005). "High-Precision Ephemerides of Planets—EPM and Determination of Some Astronomical Constants". Solar System Research (Springer Science+Business Media) 39 (3): 184. doi:10.1007/s11208-005-0033-2. Bibcode: 2005SoSyR..39..176P.
14. ↑ Berdeu, Anthony; Langlois, Maud; Vachier, Frédéric (February 2021). "First observation of a quadruple asteroid. Detection of a third moon around (130) Elektra with SPHERE/IFS". Astronomy & Astrophysics. 658: 21.
15. ↑ Michalak, G. (2001). "Determination of asteroid masses". Astronomy & Astrophysics 374 (2): 703–711. doi:10.1051/0004-6361:20010731. Bibcode: 2001A&A...374..703M. http://www.aanda.org/index.php?option=article&access=standard&Itemid=129&url=/articles/aa/abs/2001/29/aa10228/aa10228.html. Retrieved 2008-11-10.
16. ↑ Michalak, G. (2001), assumed masses of perturbing asteroids used in calculations of perturbations of the test asteroids.[clarification needed]
17. ↑ Martinez, Patrick (1994). The Observer's Guide to Astronomy. Cambridge University Press. p. 298.
18. ↑ "(99942) Apophis Ephemerides for 13 Apr 2029". NEODyS (Near Earth Objects Dynamic Site). https://newton.spacedys.com/neodys/index.php?pc=1.1.3.1&n=99942&oc=500&y0=2029&m0=4&d0=13&h0=18&mi0=0&y1=2029&m1=4&d1=14&h1=0&mi1=0&ti=10&tiu=minutes.
19. ↑ "Minor Planet Ephemeris Service: Query Results". https://www.minorplanetcenter.net/cgi-bin/mpeph2.cgi?ty=e&TextArea=Apophis&d=2029+Apr.+13+20:30&l=60&i=1&u=m&uto=0&c=&long=&lat=&alt=&raty=a&s=t&m=m&adir=S&oed=&e=-2&resoc=&tit=&bu=&ch=c&ce=f&js=f.
20. ↑ "JPL Small-Body Database Search Engine: Asteroids and i > 90 (deg)". http://ssd.jpl.nasa.gov/sbdb_query.cgi?obj_group=all;obj_kind=ast;obj_numbered=all;OBJ_field=0;ORB_field=0;c1_group=ORB;c1_item=Bj;c1_op=>;c1_value=90;table_format=HTML;max_rows=200;format_option=comp;c_fields=AcBhBgBjBiBnBsCjCpAi;.cgifields=format_option;.cgifields=obj_kind;.cgifields=obj_group;.cgifields=obj_numbered;.cgifields=ast_orbit_class;.cgifields=table_format;.cgifields=com_orbit_class&query=1&c_sort=AcA.
21. ↑ Morais, M.H.M.; F. Namouni (2013). "Asteroids in retrograde resonance with Jupiter and Saturn". Monthly Notices of the Royal Astronomical Society Letters 436: L30–L34. doi:10.1093/mnrasl/slt106. Bibcode: 2013MNRAS.436L..30M.
22. ↑ 2008 DG8 and Ceres in 1930
23. ↑ 1999 LE31 approaches to Jupiter and Saturn
24. ↑ Chang'E 2 images of Toutatis – December 13, 2012 – The Planetary Society
25. ↑ "1994 Release #9412" (Press release). NASA. 1994-02-18. Retrieved 2008-04-17.
26. ↑ "Sentry: Earth Impact Monitoring | 29075 (1950 DA) Earth Impact Risk Summary". 24 January 2025. https://cneos.jpl.nasa.gov/sentry/details.html#?des=29075.
27. ↑ "Archived copy". http://pdssbn.astro.umd.edu/SBNast/archive/DISCOVER/discnote.tab.

## External links

* Lists and plots: Minor Planets
* PDS Asteroid Data Archive
* SBN Small Bodies Data Archive
* NASA Near Earth Object Program
* Major News About Minor Objects
* Latest News About Asteroids & Meteorites

* v
* t
* e

Asteroids

Main|

* Notable asteroids
* Physical characteristics
* dynamic method
* Impact avoidance
* Tracking
* Capture
* Gravitational keyhole
* Earth-crosser
* Close approaches
* Binary
* moon
* contact
* P–L

Distribution|

* Interior to Earth
* vulcanoids
* Mercury-crossers
* Venus-crossers
* Main-belt
* Kirkwood gap
* comets
* Trojans
* Venus trojan
* Earth
* Mars
* Jupiter
* Uranus trojan
* Neptune trojan
* Near-Earth
* Aten
* Amor
* Apollo
* Apohele
* Earth-crossers
* Between Earth and the main belt
* Mars crossers
* Mars trojans
* Outer Solar System, does not include distant minor planets
* Jupiter-crossers
* Jupiter trojan

Classification|

| Orbital|

* Group
* Family
* (list)

|

Spectral|

| Tholen|

* C-group
* B-type
* F-type
* G-type
* C-type
* S-type
* X-group
* M-type
* E-type
* P-type
* small classes
* A-type
* D-type
* J-type
* T-type
* Q-type
* R-type
* V-type

|

SMASS|

* C-group
* B-type
* C-type
* Cg
* Ch
* Cgh
* Cb
* S-group
* A-type
* Q-type
* R-type
* K-type
* L-type
* S-type
* Sa
* Sq
* Sr
* Sk
* Sl
* X-group
* X-type
* Xe
* Xc
* Xk
* small types
* T-type
* D-type
* Ld-type
* O-type
* V-type

Exploration|

* Asteroid Redirect Mission
* Asteroids visited by spacecraft
* Mining
* Ceres
* Colonization
* Near-Earth Object Surveillance Mission

Lists|

* Near-Earth
* Minor planets
* Lost
* Discovering observatories
* Space missions

* See also: Asteroids in fiction
* Asteroids in astrology
* occultation
* Comet
* Minor planet

* Category

0.00

(0 votes)

Original source: https://en.wikipedia.org/wiki/List of exceptional asteroids. Read more

|

Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:List_of_exceptional_asteroids&oldid=4342227"
*[v]: View this template
*[t]: Discuss this template
*[e]: Edit this template