List of nearest exoplanets

Short description: none

Epsilon Indi Ab, 12 light-years away, with its parent star Epsilon Indi A blacked out, as pictured by JWST in 2023.[1] Distribution of nearest known exoplanets as of March 2018

There are 4,160 known exoplanets, or planets outside the Solar System that orbit a star, as of January 1, 2020; only a small fraction of these are located in the vicinity of the Solar System.[2] Within 10 parsecs (32.6 light-years), there are 106 exoplanets listed as confirmed by the NASA Exoplanet Archive.[note 1][3] Among the over 500 known stars and brown dwarfs within 10 parsecs,[4][note 2] around 60 have been confirmed to have planetary systems; 51 stars in this range are visible to the naked eye,[note 3][6] eight of which have planetary systems.

The first report of an exoplanet within this range was in 1998 for a planet orbiting around Gliese 876 (15.3 light-years (ly) away), and the latest as of 2026 is a system around Gliese 725 B (11.5 ly). The closest exoplanets are those found orbiting the star closest to the Solar System, which is Proxima Centauri 4.25 light-years away. The first confirmed exoplanet discovered in the Proxima Centauri system was Proxima Centauri b, in 2016. HD 219134 (21.6 ly) has six exoplanets, the highest number discovered for any star within this range.

Most known nearby exoplanets orbit close to their stars. A majority are significantly larger than Earth, but a few have similar masses, including planets around YZ Ceti, Gliese 367, Proxima Centauri, and Barnard's Star which may be less massive than Earth. Several confirmed exoplanets are hypothesized to be potentially habitable, with Proxima Centauri b and GJ 1002 b (15.8 ly) considered among the most likely candidates.[7] The International Astronomical Union has assigned proper names to some known extrasolar bodies, including nearby exoplanets, through the NameExoWorlds project. Planets named in the 2015 event include the planets around Epsilon Eridani (10.5 ly) and Fomalhaut,[note 4][10] while planets named in the 2022 event include those around Gliese 436, Gliese 486, and Gliese 367.[11]

## Contents

* 1 Exoplanets within 10 parsecs
* 2 Excluded objects
* 3 See also
* 4 Notes
* 5 References
* 6 External links

## Exoplanets within 10 parsecs

Key to colors  ° | Mercury, Earth and Jupiter (for comparison purposes)

|

# | Confirmed multiplanetary systems
↑ | Exoplanets believed to be potentially habitable[7]
Confirmed exoplanets[3] Host star system | Companion exoplanet (in order from star)  | Notes and additional planetary observations

|
|

Name  | Distance
(ly)
| Apparent
magnitude
(V)  | Mass
(M☉)
| Label
[note 5] | Mass
(M⊕)[note 6]
| Radius
(R⊕)
| Semi-major axis
(AU)
| Orbital period
(days)
| Eccentricity
| Inclination
(°)
| Discovery
method | Discovery year
Sun° | 0.000016 | -26 −26.7 | rowspan = "3"|1 | b0 Mercury | 0000.0550 0.055

|| 0.3829 || 0.387 || 0088 88.0

|| 0.205 || 3.38 || — || 1 —

| For comparison purposes. One candidate planet
d0 Earth | 0001.0000 1

|| 1 || 1 || 0365 365.3

|| 0.0167 || 7.25 || — || 0 —

f0 Jupiter | 0317.8000 317.8

|| 10.9 10.973

|| 5.20 || 4333 4,333

|| 0.0488 || 6.09 || — || 1 —

Proxima Centauri# | 4.2465 | 1113 11.13  | rowspan="2" | 0.123  | d | 0000.2600 ≥0.26  | ~0.81 ± 0.08 | 0.0289 | 5.122 | 0.04 | — | RV | 2025  | [13][14][15] one disputed candidate (c)[16][17][18][19]
b↑ | 0001.0700 ≥1.055  | 0.94 - 1.4 | 0.0486 | 11.19 | 0.02 | — | RV | 2016
Barnard's Star# | 5.9629 | 9.51 | 0.162  | d | 0000.2630 ≥0.26  | — | 0.0188 | 2.340 | 0.04 | — | RV | 2025  | [20]
b | 0000.2990 ≥0.30  | — | 0.0229 | 3.154 | 0.03 | — | RV | 2024
c | 0000.3350 ≥0.34  | — | 0.0274 | 4.124 | 0.08 | — | RV | 2025
e | 0000.1930 ≥0.19  | — | 0.0381 | 6.739 | 0.04 | — | RV | 2025
Lalande 21185# | 8.304 | 0752 7.52  | rowspan="2"| 0.46  | b | 0002.6900 ≥2.69  | — | 0.0788 | 12.94 | 0.06 | — | RV | 2019  | 1 candidate[21]
c | 0013.6000 ≥13.6  | — | 2.94 | 2946 2,946  | 0.13 | — | RV | 2021
Epsilon Eridani | 10.501 | 0373 3.73  | 0.82  | b0 Ægir | 318 | — | 3.53 | 2,680 | 0.06 | 40 | RV | 2000  | [22] 1 inferred planet, 1 or possibly 2 inner debris discs, and an outer disc[23]
Gliese 887# | 10.724 | 0734 7.34  | rowspan="4"| 0.489  | e | 0001.4600 ≥1.46  | — | 0.042 | 4.42 | – | — | RV | 2026  | [24] 2 candidates[25][26]
b | 0003.9000 ≥3.9  | — | 0.068 | 9.262 | 0.14 | — | RV | 2019
c | 0006.5000 ≥6.5  | — | 0.121 | 21.78 | 0.17 | — | RV | 2019
d↑ | 0006.1000 ≥6.1  | — | 0.212 | 50.77 | 0.25 | — | RV | 2026
Ross 128 | 11.007 | 1110 11.1  | 0.168  | b↑ | 0001.4000 ≥1.40  | style="background:#BCD4E6;" | — | 0.0496 | 9.866 | 0.12 | — | RV | 2017  | [27]
Gliese 725 A  | 11.491  | 8.94  | 0.330  | b | ≥2.78  | —  | 0.068  | 11.2201  | 0.0  | —  | RV | 2024  | [28]
Gliese 725 B  | 11.491  | 9.70  | 0.25  | c | ≥3.4  | —  | 0.139  | 37.90  | —  | —  | RV | 2025  | [29]
Groombridge 34 A# | 11.619 | 0810 8.1  | rowspan="2"|0.38  | b | 0003.0300 ≥3.03  | — | 0.072 | 11.44 | 0.09 | ~54? | RV | 2014  | [30][31]
c | 0036.0000 ≥36  | — | 5.4 | 7600 7,600  | 0.27 | ~54? | RV | 2018
Epsilon Indi A  | 11.867 | 483 4.83  | 0.762  | b | 2005 | — | 28.4 | 63400 63,400  | 0.40 | 103.7 | RV | 2018  | nearest exoplanet directly imaged[32][33]
GJ 1061# | 11.984 | 752 7.52  | rowspan = "3" | 0.113  | b | 0001.3700 ≥1.37  | — | 0.021 | 3.204 | <0.31 | — | RV | 2019  | two solutions for d's orbit[34]
c↑ | 0001.7400 ≥1.74  | — | 0.035 | 6.689 | <0.29 | — | RV | 2019
d↑ | 0001.6400 ≥1.64  | — | 0.054 | 13.03 | <0.53 | — | RV | 2019
YZ Ceti# | 12.122 | 1210 12.1  | rowspan = "3" | 0.130  | b | 0000.7000 ≥0.70  | — | 0.0163 | 2.021 | 0.06 | — | RV | 2017  | [35]
c | 0001.1400 ≥1.14  | — | 0.0216 | 3.060 | 0.0 | — | RV | 2017
d | 0001.0900 ≥1.09  | — | 0.0285 | 4.656 | 0.07 | — | RV | 2017
Luyten's Star# | 12.348 | 1194 11.94  | rowspan="2" | 0.29  | c | 0001.1800 ≥1.18  | — | 0.0365 | 4.723 | 0.10 | — | RV | 2017  | 2 candidates[36][37]
b↑ | 0002.8900 ≥2.89  | — | 0.0911 | 18.65 | 0.17 | — | RV | 2017
Teegarden's Star# | 12.497 | 1540 15.40  | rowspan="3" | 0.08  | b↑ | 0001.1600 ≥1.16  | style="background:#BCD4E6;" | — | 0.0259 | 4.906 | 0.03 | — | RV | 2019  | [38][39]
c↑ | 0001.0500 ≥1.05  | — | 0.0455 | 11.42 | 0.04 | — | RV | 2019
d | 0000.8200 ≥0.82  | — | 0.0791 | 26.13 | 0.07 | — | RV | 2024
Wolf 1061# | 14.050 | 1010 10.1  | rowspan="3" | 0.25  | b | 0001.9100 ≥1.91  | — | 0.0375 | 4.887 | 0.15 | — | RV | 2015  | [36]
c↑ | 0003.4100 ≥3.41  | — | 0.0890 | 17.87 | 0.11 | — | RV | 2015
d | 0007.7000 ≥7.7  | — | 0.470 | 217 | 0.55 | — | RV | 2015
TZ Arietis | 14.578 | 1229.8 12.30  | 0.14  | b | 0067.0000 ≥67  | — | 0.88 | 771 | 0.46 | — | RV | 2019  | 2 refuted candidates[37][40][41]
Gliese 687# | 14.839 | 0915 9.15  | rowspan="2" |0.41  | b | 0017.2000 ≥17.2  | — | 0.163 | 38.14 | 0.17 | — | RV | 2014  | [37][40]
c | 0016.0000 ≥16.0  | — | 1.165 | 728 | 0.40 | — | RV | 2019
Gliese 674 | 14.849 | 0938 9.38  | 0.35  | b | 0011.0900 ≥11.1  | — | 0.039 | 4.694 | 0.20 | — | RV | 2007  | [42]
Gliese 876# | 15.238 | 1020 10.2  | rowspan = "4"|0.33  | d | 6.68 | — | 0.0210 | 1.938 | 0.04 | 56.7 | RV | 2005  | [43]
c | 235 | — | 0.1309 | 30.10 | 0.26 | 56.7 | RV | 2000
b | 749 | — | 0.2098 | 61.10 | 0.03 | 56.7 | RV | 1998
e | 16 | — | 0.3355 | 123.6 | 0.05 | 56.7 | RV | 2010
GJ 1002# | 15.806 | 1384 13.84  | rowspan = "2"|0.12  | b↑ | 0001.0800 ≥1.08  | style="background:#BCD4E6;" | — | 0.0457 | 10.35 | — | — | RV | 2022  | [44]
c↑ | 0001.3600 ≥1.36  | — | 0.0738 | 21.2 | — | — | RV | 2022
Gliese 832 | 16.200 | 0867 8.67  | 0.45  | b | 315 | — | 3.7 | 3853 3,853  | 0.05 | 51 or 134 | RV | 2008  | 1 refuted candidate[45][46]
GJ 3323# | 17.531 | 1220 12.2  | rowspan = "2" | 0.164  | b | 0002.0200 ≥2.0  | — | 0.0328 | 0005.36 5.36  | 0.23 0.2  | — | RV | 2017  | [36]
c | 0002.3100 ≥2.3  | — | 0.126 | 0040.5 40.5  | 0.17 0.2  | — | RV | 2017
Gliese 251# | 18.215 | 0965 9.65  | rowspan = "2" | 0.372  | b | 0003.8500 ≥3.85  | — | 0.0808 | 0014.2370 14.2370  | — | — | RV | 2020  | [47][48]
c | 0003.8400 ≥3.84  | — | 0.196 | 0053.647 53.647  | — | — | RV | 2025
Gliese 752 A  | 19.292 | 0913 9.13  | 0.46  | b | 0012.2140 ≥12.2  | — | 0.343 | 0105.9 106  | 0.10 | — | RV | 2018  | [49][50]
82 G. Eridani# | 19.704 | 0426 4.26  | rowspan = "3"|0.79  | b | 0002.1500 ≥2.15  | — | 0.126 | 0018.3140 18.3  | 0.06 | — | RV | 2011  | [51]
c | 0002.9800 ≥2.98  | — | 0.363 | 0089.68 89.7  | 0.08 | — | RV | 2011
d↑ | 0005.8200 ≥5.82  | style="background:#BCD4E6;" | — | 1.354 | 0647.6 648  | style="background:#BCD4E6;" | 0.45 | — | RV | 2023
HN Librae | 20.395 | 1131.7 11.32  | 0.29  | b | 0005.4600 ≥5.5  | — | 0.142 | 0036.116 36.1  | 0.08 | — | RV | 2023  | 1 candidate[52]
EQ Pegasi A  | 20.400 | 1038 10.38  | 0.436  | b | 0718 718  | — | 0.643 | 0284.39 284  | 0.35 | 69.2 | Astrometry | 2022  | [53]
Gliese 581# | 20.549 | 1055 10.5  | rowspan = "3"|0.295  | e | 0002.4800 2.5  | — | 0.0280 | 0003.1481 3.15  | 0.01 | 47 | RV | 2009  | 3 refuted candidates and a disc[54]
b | 0020.5000 20.5  | — | 0.0399 | 0005.3686 5.37  | 0.03 | 47 | RV | 2005
c | 0006.8100 6.8  | — | 0.0718 | 0012.9211 12.9  | 0.03 | 47 | RV | 2007
Gliese 338 B  | 20.658 | 0700 7.0  | 0.64  | b | 0010.27000 ≥10.3  | — | 0.141 | 0024.45 24.5  | 0.11 | — | RV | 2020  | [55]
Gliese 625 | 21.131 | 1020 10.2  | 0.30  | b | 0002.82000 ≥2.8  | — | 0.0784 | 0014.6 14.6  | 0.13 ~0.1  | — | RV | 2017  | [56]
HD 219134# | 21.336 | 0557 5.57  | rowspan = "5"|0.78  | b | 0004.7400 4.7  | 1.60 | 0.0388 | 00031 3.09  | 0 ~0  | 85.05 | RV | 2015  | [57][58][59] Has 1 candidate planet (g)[60]
c c | 0004.3600 4.4  | 1.51 | 0.065 | 00068 6.77  | 0.0620 0.062  | 87.28 | RV | 2015
f f | 0007.3000 ≥7.3  | — | 0.146 | 0023 22.7  | 0.148 0.148  | ~87? | RV | 2015
d d | 0016.1700 ≥16  | — | 0.237 | 0047 46.9  | 0.138 0.138  | ~87? | RV | 2015
h h (e)  | 0108.0000 ≥108  | — | 3.11 | 2247 2,247  | 0.06 0.06  | ~87? | RV | 2015
LTT 1445 A# | 22.387 | 1052.9 10.53  | rowspan="2"| 0.26  | c | 0001.5400 1.54  | 1.15 | 0.0266 | 0003.12390 3.12  | <0.22 | 87.43 | Transit | 2021  | 1 candidate[61][62][63]
b | 0002.8700 2.87  | 1.30 | 0.0381 | 0005.35877 5.36  | <0.11 | 89.68 | Transit | 2019
Gliese 393 | 22.953 | 0865 8.65  | 0.41  | b | 0001.7100 ≥1.71  | — | 0.0540 | 0007.0268 7.03  | 0.00 | — | RV | 2019  | [37][64]
GJ 4274# | 23.596 | 1332 13.3  | rowspan = "2"|0.18  | b3 b  | 0002.9500 ≥2.95  | — | 0.0153 | 0001.6339 1.6339  | 0.003 | — | RV | 2026  | [65]
c3 c  | 0008.6700 ≥8.67  | — | 0.187 | 0069.525 69.525  | 0.01 | — | RV | 2026
Gliese 667 C# | 23.623 | 1022 10.2  | rowspan = "2"|0.33  | b3 b | 0005.4000 ≥5.4  | — | 0.049 | 0007.20 7.20  | 0.13 | ~52? | RV | 2009  | 5 dubious candidates
[66][7][67][68][37]
c3 c

↑ || 0003.9000 ≥3.9

| — | 0.1251 | 0028.2 28.2  | 0.03 | ~52? | RV | 2011
Gliese 514 | 24.878 | 0903 9.03  | 0.53  | b | 0005.2000 ≥5.2  | — | 0.421 | 140 | 0.45 | — | RV | 2022  | [69]
GJ 1151 | 26.231 | 1401 14.01  | 0.164  | c | 0010.6200 ≥10.6  | — | 0.571 | 390 | — | — | RV | 2023
Gliese 486 | 26.351 | 1139.5 11.395  | 0.32  | b0 Su | 0002.8200 2.8  | 1.31 | 0.0173 | 0001.47 1.47  | 0 <0.05  | 88.4 | Transit | 2021  | [70]
Gliese 686 | 26.613 | 0958 9.58  | 0.42  | b | 0007.1000 ≥7.1  | — | 0.097 | 0015.5 15.5  | 0.04 | — | RV | 2019  | [71][37]
GJ 1289 | 27.275 | 12.67[72] | 0.21  | b | 0006.27 ≥6.3  | — | 0.27 | 112 | 0 | — | RV | 2024  | [73]
61 Virginis# | 27.836 | 0474 4.74  | rowspan = "3"|0.95  | b | 0006.1000 ≥6.1  | — | 0.05 | 0004.215 4.22  | 0.05 | ~77? | RV | 2009  | a debris disc[74]
c | 0017.9000 ≥17.9  | — | 0.22 | 0038.09 38.1  | 0.06 | ~77? | RV | 2009
d | 0010.5000 ≥10.5  | — | 0.47 | 0123.2 123  | 0.12 | ~77? | RV | 2009
CD Ceti | 28.052 | 1400.1 14.001  | 0.161  | b | 0003.9500 ≥3.95  | — | 0.0185 | 0002.2907 2.29  | 0 | — | RV | 2020  | [75]
HD 192310# | 28.739 | 0613 6.13  | rowspan = "2"|0.78  | b | 0016.9000 ≥17  | — | 0.32 | 0074.7 75  | 0.13 | — | RV | 2010  | [76]
c | 0024.0000 ≥24  | — | 1.18 | 0526 530  | 0.32 ~0.3  | — | RV | 2011
Gliese 849# | 28.750 | 1042 10.4  | rowspan = "2"|0.49  | b | 0269.9000 ≥270  | — | 2.26 | 1905 1,910  | 0.05 | — | RV | 2006  | [77][37]
c | 0300.0000 ≥300  | — | 4.82 | 5520 5,520  | 0.087 | — | RV | 2006
Gliese 433# | 29.605 | 0979 9.79  | rowspan="3"|0.48  | b | 0006.0000 ≥6.0  | — | 0.062 | 00074 7.37  | 0.04 | — | RV | 2009  | [78][37][79]
d | 0005.2000 ≥5.2  | — | 0.178 | 00036.1 36.1  | 0.07 | — | RV | 2020
c | 0032.4200 ≥32  | — | 4.82 | 05094 5,090  | 0.12 | — | RV | 2012
Gliese 367# | 30.719 | 0998 9.98  | rowspan="3"|0.45  | b0 Tahay | 0000.6330 0.63  | 0.70 | 0.0071 | 0000.3219225 0.322  | 0.06 | 79.89 | Transit | 2021  | [80][81]
c | 0004.1300 ≥4.1  | — | 0.077 | 11.5 | 0.09 | ~80? | RV | 2023
d | 0006.0300 ≥6.0  | — | 0.159 | 34.4 | 0.14 | ~80? | RV | 2023
Gliese 357# | 30.776 | 1090 10.9  | rowspan="3"|0.34  | b | 0006.1000 6.1  | 1.17 | 0.035 | 3.93 | 0.02 | 88.92 | Transit | 2019  | [82][37]
c | 0003.6000 ≥3.6  | — | 0.061 | 9.13 | 0.04 | ~89? | RV | 2019
d↑ | 0007.7000 ≥7.7  | — | 0.204 | 55.7 | 0.03 | ~89? | RV | 2019
Gliese 176 | 30.937 | 1010 10.1  | 0.45  | b | 0008.0000 ≥8.0  | — | 0.066 | 0008.77 8.77  | 0.08 | — | RV | 2007  | 1 disputed candidate[83][84][37]
GJ 3512# | 30.976 | 1505 15.1  | rowspan="2" | 0.123  | b | 0146.7000 ≥147  | — | 0.338 | 204 | 0.44 | — | RV | 2019  | [85][86]
c | 0143.0000 ≥143  | — | 1.722 | 2350 2,350  | — | — | RV | 2020
G 192-15# | 31.075 | 1453 14.5  | rowspan="2" | 0.132  | b | 0001.0300 ≥1.03  | — | 0.0172 | 2.275 | 0 | — | RV | 2025  | [86]
c | 0014.3000 ≥14.3  | — | 1.137 | 1219 1,219  | 0.68 | — | RV | 2025
Wolf 1069 | 31.229 | 1399 13.99  | 0.167  | b↑ | 0001.2600 ≥1.26  | style="background:#BCD4E6;" | — | 0.0672 | 15.56 | — | — | RV | 2023  | [87]
AU Microscopii# | 31.683 | 0863 8.63  | rowspan="2"| 0.50  | b | 0006.3000 6.3  | 4.38 | 0.0645 | 0008.4629991 8.463  | 0.10 | 89.03 | Transit | 2020  | [88] 2 candidates[89][90][91][92]
c | 0011.3000 11.3  | 3.51 | 0.1101 | 18.858991 18.86  | 0 | 88.62 | Transit | 2020
Gliese 436 | 31.882 | 1067 10.67  | 0.41  | b0 Awohali | 0021.3600 21.4  | 4.33 | 0.0280 | 2.64 | 0.15 | 85.8 | RV | 2004  | [93][94] One dubious candidate (UCF-1.01)[95]
G 268-110  | 31.888 | 1447 14.5  | 0.137  | b | 0001.5200 ≥1.52  | — | 0.0128 | 1.433 | 0 | — | RV | 2025  | [86]
Gliese 49 | 32.158 | 0890 8.9  | 0.57  | b | 0005.6300 ≥5.63  | — | 0.0905 | 13.8508 | 0.363 | — | RV | 2019  | [96]
GJ 3988  | 32.316 | 1363 13.6  | 0.184  | b | 0003.6900 ≥3.7  | — | 0.0405 | 6.944 | 0 | — | RV | 2023  | [97]
HD 260655# | 32.608 | 0977 9.77  | rowspan="2"| 0.439  | b | 0002.1400 2.14  | 1.240 | 0.0293 | 0002.76953 2.780  | 0.039 | 87.35 | Transit | 2022  | [98]
c | 0003.0900 3.09  | 1.533 | 0.0475 | 0005.70588 5.706  | 0.038 | 87.79 | Transit | 2022

## Excluded objects

Unlike for bodies within the Solar System, there is no clearly established method for officially recognizing an exoplanet. According to the International Astronomical Union, an exoplanet should be considered confirmed if it has not been disputed for five years after its discovery.[99] There have been examples where the existence of exoplanets has been proposed, but even after follow-up studies their existence is still considered doubtful by some astronomers. Such cases include Wolf 359 (7.9 ly, in 2019),[37] Tau Ceti (11.9 ly, in 2012 & 2017),[100] Gliese 682 (16.3 ly, in 2014),[79] and HD 102365 A (30.4 ly, in 2011).[100] There are also several instances where proposed exoplanets were later disproved by subsequent studies, including candidates around Alpha Centauri B (4.36 ly),[101] Kapteyn's Star (12.8 ly),[102] Van Maanen 2 (14.1 ly),[103] Groombridge 1618 (15.9 ly),[104] AD Leonis (16.2 ly),[105] 40 Eridani A (16.3 ly),[106][107] Gliese 229 A (18.8 ly),[108] VB 10 (19.3 ly),[109] and Fomalhaut (25.1 ly).[110]

A candidate planet around LHS 288 was proposed in 2007, but it has not been confirmed.[111] In 2021, a candidate planet was detected around Vega, though it has yet to be confirmed.[112] Another candidate planet, Candidate 1, was directly imaged around Alpha Centauri A, though it may also be a clump of asteroids or an artifact of the discovery mechanism.[113] Candidate planets around Luyten 726-8 (8.77 ly), GJ 3378 (25.2 ly) and Achird (19.3 ly) were reported in 2024, 2024 and 2025, respectively.[114][73][115]

The Working Group on Extrasolar Planets of the International Astronomical Union adopted in 2003 a working definition on the upper limit for what constitutes a planet: not being massive enough to sustain thermonuclear fusion of deuterium. Some studies have calculated this to be somewhere around 13 times the mass of Jupiter, and therefore objects more massive than this are usually classified as brown dwarfs.[116] Some proposed candidate exoplanets have been shown to be massive enough to fall above the threshold, and thus are likely brown dwarfs, as is the case for: SCR 1845-6357 B (13.1 ly),[117] SDSS J1416+1348 B (30.3 ly),[118] and WISE 1217+1626 B (30 ly).[119]

Excluded from the current list are known examples of potential free-floating sub-brown dwarfs, or "rogue planets", which are bodies that are too small to undergo fusion yet they do not revolve around a star. Known such examples include: WISE 0855−0714 (7.4 ly),[120] UGPS 0722-05, (13.4 ly)[121] WISE 1541−2250 (18.6 ly),[122] and SIMP J01365663+0933473 (20.0 ly).[123]

## See also

* List of nearest stars and brown dwarfs
* List of nearest bright stars
* List of nearest terrestrial exoplanet candidates
* Lists of planets
* List of planet types
* List of potentially habitable exoplanets
* Lists of astronomical objects

## Notes

1. ↑ Listed values are primarily taken from NASA Exoplanet Archive,[3] but other databases include a few additional exoplanet entries tagged as "Confirmed" that have yet to be compiled into the NASA archive. Such databases include:

"Exoplanet Catalog". Extrasolar Planets Encyclopaedia. 1995. Full table. https://exoplanet.eu/catalog/.
"Exoplanets Data Explorer". California Planet Survey. Click the "+" button to visualize additional parameters. http://exoplanets.org/table/.
"Open Exoplanet Catalogue". Click the "Show options" to visualize additional parameters. http://www.openexoplanetcatalogue.com/systems/.
2. ↑ For reference, the 100th closest known star system in April 2021 was EQ Pegasi (20.4 ly).[4]
3. ↑ According to the Bortle scale, an astronomical object is visible to the naked eye under "typical" dark-sky conditions in a rural area if it has an apparent magnitude smaller than +6.5. To the unaided eye, the limiting magnitude is +7.6 to +8.0 under "excellent" dark-sky conditions (with effort).[5]
4. ↑ The star Epsilon Eridani was named Ran (after Rán, the Norse goddess of the sea), and the planet Epsilon Eridani b was named AEgir (after Ægir, Rán's husband),[8] while the planet Fomalhaut b was named Dagon (after Dagon, an ancient Syrian “fish god”[9]).[10]
5. ↑ Exoplanet naming convention assigns uncapitalized letters starting from b to each planet based on chronological order of their initial report, and in increasing order of distance from the parent star for planets reported at the same time. Omitted letters signify planets that have yet to be confirmed, or planets that have been retracted altogether.
6. ↑ Most reported exoplanet masses have very large error margins (typically, between 10% and 30%). The mass of an exoplanet has generally been inferred from measurements on changes in the radial velocity of the host star, but this kind of measurement only allows for an estimate on the exoplanet's orbital parameters, but not on their orbital inclination (i). As such, most exoplanets only have an estimated minimum mass (Mreal*sin(i)), where their true masses are statistically expected to come close to this minimum, with only about 13% chance for the mass of an exoplanet to be more than double its minimum mass.[12]

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77. ↑ "GJ 849". California Institute of Technology. https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=GJ+849.
78. ↑ "GJ 433". California Institute of Technology. https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=GJ+433.
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83. ↑ "HD 285968". California Institute of Technology. https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=HD+285968.
84. ↑ "GJ 176 c". Extrasolar Planets Encyclopaedia. 2010-12-17. https://exoplanet.eu/catalog/gj_176_c--786/. Retrieved 2014-05-20.
85. ↑ Morales, J. C. et al. (2019). "A giant exoplanet orbiting a very-low-mass star challenges planet formation models". Science 365 (6460): 1441–1445. doi:10.1126/science.aax3198. ISSN 0036-8075. PMID 31604272. Bibcode: 2019Sci...365.1441M.
86. ↑ 86.0 86.1 86.2 Kaminski, A. et al. (March 2025). "The CARMENES search for exoplanets around M dwarfs. Occurrence rates of Earth-like planets around very low-mass stars". Astronomy & Astrophysics 696: A101. doi:10.1051/0004-6361/202453381. Bibcode: 2025A&A...696A.101K.
87. ↑ Kossakowski, D. et al. (January 2023). "The CARMENES search for exoplanets around M dwarfs, Wolf 1069 b: Earth-mass planet in the habitable zone of a nearby, very low-mass star". Astronomy & Astrophysics 670. doi:10.1051/0004-6361/202245322. Bibcode: 2023A&A...670A..84K.
88. ↑ Donati, J.-F.; Cristofari, P. I.; Moutou, C.; L’Heureux, A.; Cook, N. J.; Artigau, E.; Alencar, S. H. P.; Gaidos, E. et al. (2025). "Six-year SPIRou monitoring of the young planet-host AU Mic". Astronomy & Astrophysics (EDP Sciences) 700: A227. doi:10.1051/0004-6361/202555371. ISSN 0004-6361. Bibcode: 2025A&A...700A.227D.
89. ↑ Plavchan, Peter et al. (2020). "A planet within the debris disk around the pre-main-sequence star AU Microscopii". Nature 582 (7813): 497–500. doi:10.1038/s41586-020-2400-z. PMID 32581383. Bibcode: 2020Natur.582..497P.
90. ↑ Martioli, E. (2021). "New constraints on the planetary system around the young active star AU Mic. Two transiting warm Neptunes near mean-motion resonance". Astronomy & Astrophysics A177: 649. doi:10.1051/0004-6361/202040235. Bibcode: 2021A&A...649A.177M.
91. ↑ Wittrock, Justin M. et al. (2023), "Validating AU Microscopii d with Transit Timing Variations", The Astronomical Journal 166 (6): 232, doi:10.3847/1538-3881/acfda8, Bibcode: 2023AJ....166..232W
92. ↑ Donati, J-F; Cristofari, P I; Finociety, B et al. (24 April 2023). "The magnetic field and multiple planets of the young dwarf AU Mic". Monthly Notices of the Royal Astronomical Society 525: 455–475. doi:10.1093/mnras/stad1193. ISSN 0035-8711.
93. ↑ Gillon, M. (2007). "Detection of transits of the nearby hot Neptune GJ 436 b". Astronomy and Astrophysics 472 (2): L13–L16. doi:10.1051/0004-6361:20077799. Bibcode: 2007A&A...472L..13G.
94. ↑ Lanotte, A. A. et al. (2014). "A global analysis of Spitzer and new HARPS data confirms the loneliness and metal-richness of GJ 436 b". Astronomy and Astrophysics 572: A73. doi:10.1051/0004-6361/201424373. Bibcode: 2014A&A...572A..73L.
95. ↑ Stevenson, Kevin B. et al. (2014). "A Hubble Space Telescope Search for a Sub-Earth-sized Exoplanet in the GJ 436 System". The Astrophysical Journal 796 (1): 32. doi:10.1088/0004-637X/796/1/32. Bibcode: 2014ApJ...796...32S.
96. ↑ Perger, M. et al. (April 2019). "Gliese 49: Activity evolution and detection of a super-Earth". Astronomy & Astrophysics 624: 19. doi:10.1051/0004-6361/201935192. A123. ISSN 0004-6361. Bibcode: 2019A&A...624A.123P.
97. ↑ Gorrini, P. et al. (December 2023). "Planetary companions orbiting the M dwarfs GJ 724 and GJ 3988. A CARMENES and IRD collaboration". Astronomy & Astrophysics 680: A28. doi:10.1051/0004-6361/202347108. Bibcode: 2023A&A...680A..28G.
98. ↑ Luque, R. et al. (2022). "The HD 260655 system: Two rocky worlds transiting a bright M dwarf at 10 pc". Astronomy & Astrophysics 664: A199. doi:10.1051/0004-6361/202243834. Bibcode: 2022A&A...664A.199L.
99. ↑ Lee, Rhodi (2015-09-18). "Want To Name An Exoplanet? Here's Your Chance". Tech Times. http://www.techtimes.com/articles/77119/20150818/want-to-name-an-exoplanet-heres-your-chance.htm.
100. ↑ 100.0 100.1 Figueira, P.; Faria, J. P.; Silva, A. M.; Castro-González, A.; Silva, J. Gomes da; Sousa, S. G.; Bossini, D.; Zapatero-Osorio, M. R. et al. (2025-07-10). "A comprehensive study on radial velocity signals using ESPRESSO: Pushing precision to the 10 cm/s level". Astronomy and Astrophysics 700: A174. doi:10.1051/0004-6361/202553869. Bibcode: 2025A&A...700A.174F.
101. ↑ Rajpaul, Vinesh (19 October 2015). "Ghost in the time series: no planet for Alpha Cen B". Monthly Notices of the Royal Astronomical Society: Letters 456 (1): L6–L10. doi:10.1093/mnrasl/slv164. Bibcode: 2016MNRAS.456L...6R.
102. ↑ Bortle, Anna et al. (2021). "A Gaussian Process Regression Reveals No Evidence for Planets Orbiting Kapteyn's Star". The Astronomical Journal 161 (5): 230. doi:10.3847/1538-3881/abec89. Bibcode: 2021AJ....161..230B.
103. ↑ Farihi, J.; Becklin, E. E.; Macintosh, B. A. (June 2004). "Mid-Infrared Observations of van Maanen 2: No Substellar Companion". Astrophysical Journal Letters 608 (2): L109–L112. doi:10.1086/422502. Bibcode: 2004ApJ...608L.109F.
104. ↑ Heinze, A. N.; Hinz, Philip M.; Sivanandam, Suresh et al. (2010-05-10). "Constraints on Long-period Planets from an L'- and M-band Survey of Nearby Sun-like Stars: Observations". The Astrophysical Journal 714 (2): 1551–1569. doi:10.1088/0004-637X/714/2/1551. ISSN 0004-637X. Bibcode: 2010ApJ...714.1551H.
105. ↑ Carleo, I. (June 2020). "The GAPS Programme at TNG. XXI. A GIARPS case study of known young planetary candidates: confirmation of HD 285507 b and refutation of AD Leonis b". Astronomy & Astrophysics 638: A5. doi:10.1051/0004-6361/201937369. Bibcode: 2020A&A...638A...5C.
106. ↑ Ma, Bo et al. (October 2018). "The first super-Earth detection from the high cadence and high radial velocity precision Dharma Planet Survey". Monthly Notices of the Royal Astronomical Society 480 (2): 2411–2422. doi:10.1093/mnras/sty1933. Bibcode: 2018MNRAS.480.2411M.
107. ↑ Burrows, Abigail et al. (April 2024). "The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity". The Astronomical Journal 167 (5): 243. doi:10.3847/1538-3881/ad34d5. Bibcode: 2024AJ....167..243B.
108. ↑ Deslières, Ariane; Cadieux, Charles; Doyon, René; Artigau, Étienne; Cook, Neil J.; Fontanive, Clémence; Vandal, Thomas (February 2025). "The Gl 229 System Revisited with the Line-by-line Framework: Planetary Signals Now Appear as Stellar Activity Ghosts" (in en). The Astronomical Journal 169 (3): 182. doi:10.3847/1538-3881/ada77a. ISSN 1538-3881. Bibcode: 2025AJ....169..182D.
109. ↑ "VB 10 b". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/vb_10_b--550/. Retrieved 2015-09-17.
110. ↑ Gáspár, András; Rieke, George H. (April 20, 2020). "New HST data and modeling reveal a massive planetesimal collision around Fomalhaut". PNAS 117 (18): 9712–9722. doi:10.1073/pnas.1912506117. PMID 32312810. Bibcode: 2020PNAS..117.9712G.
111. ↑ . doi:10.1086/599044. Bibcode: 2009PASP..121..365B.
112. ↑ Hurt, Spencer A.; Quinn, Samuel N.; Latham, David W.; Vanderburg, Andrew; Esquerdo, Gilbert A.; Calkins, Michael L.; Berlind, Perry; Angus, Ruth et al. (21 January 2021). "A Decade of Radial-velocity Monitoring of Vega and New Limits on the Presence of Planets". The Astronomical Journal 161 (4): 157. doi:10.3847/1538-3881/abdec8. Bibcode: 2021AJ....161..157H.
113. ↑ Wagner, K.; Boehle, A.; Pathak, P.; Kasper, M.; Arsenault, R.; Jakob, G.; Käufl, U.; Leveratto, S. et al. (2021-02-10). "Imaging low-mass planets within the habitable zone of α Centauri" (in en). Nature Communications 12 (1): 922. doi:10.1038/s41467-021-21176-6. ISSN 2041-1723. PMID 33568657. Bibcode: 2021NatCo..12..922W.
114. ↑ Abuter, R. et al. (May 2024). "Astrometric detection of a Neptune-mass candidate planet in the nearest M-dwarf binary system GJ65 with VLTI/GRAVITY". Astronomy & Astrophysics 685: L9. doi:10.1051/0004-6361/202449547. Bibcode: 2024A&A...685L...9G.
115. ↑ Giovinazzi, Mark R. et al. (2025-05-18). "The NEID Earth Twin Survey. II. Dynamical Masses in Seven High-acceleration Star Systems". The Astronomical Journal 170 (1): 52. doi:10.3847/1538-3881/add922. ISSN 0004-6256. Bibcode: 2025AJ....170...52G.
116. ↑ Boss, Alan P.; Butler, R. Paul; Hubbard, William B. et al. (2007). "Working Group on Extrasolar Planets". Proceedings of the International Astronomical Union 1 (T26A): 183. doi:10.1017/S1743921306004509. Bibcode: 2007IAUTA..26..183B.
117. ↑ "SCR 1845 b". Extrasolar Planets Encyclopaedia. 2012-04-13. https://exoplanet.eu/catalog/scr_1845_b--321/. Retrieved 2015-09-17.
118. ↑ "SDSS 141624 b". Extrasolar Planets Encyclopaedia. 2010-01-18. http://exoplanet.eu/catalog/sdss_141624_b/. Retrieved 2014-05-20.
119. ↑ "WISE 1217+16A b". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/wise_1217_16_a_b--1465/. Retrieved 2014-05-17.
120. ↑ Clavin, Whitney; Harrington, J. D. (2014-04-25). "NASA's Spitzer and WISE Telescopes Find Close, Cold Neighbor of Sun". NASA. http://www.nasa.gov/jpl/wise/spitzer-coldest-brown-dwarf-20140425/.
121. ↑ Lucas, P. W.; Tinney, C. G.; Burningham, B. et al. (2010). "The discovery of a very cool, very nearby brown dwarf in the Galactic plane". Monthly Notices of the Royal Astronomical Society 408 (1): L56–L60. doi:10.1111/j.1745-3933.2010.00927.x. Bibcode: 2010MNRAS.408L..56L.
122. ↑ Cushing, Michael C.; Kirkpatrick, J. Davy; Gelino, Christopher R. et al. (2011). "The Discovery of Y Dwarfs using Data from the Wide-field Infrared Survey Explorer (WISE)". The Astrophysical Journal 743 (1): 50. doi:10.1088/0004-637X/743/1/50. Bibcode: 2011ApJ...743...50C.
123. ↑ "Astronomers discover a free-range planet with incredible magnetism". 3 August 2018. https://www.astronomy.com/news/2018/08/free-range-planet.

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## External links

* "Extrasolar Planets". Planetary.org. https://www.planetary.org/explore/space-topics/exoplanets/.
* "Extrasolar Planets News". https://www.sciencedaily.com/news/space_time/extrasolar_planets/.
* "Exoplanet Exploration: Planets Beyond our Solar System". NASA. 2015-12-16. https://exoplanets.nasa.gov/.
* "Universe - Exoplanets (pictures, video, facts & news)". BBC. http://www.bbc.co.uk/science/space/universe/sights/extrasolar_planets.
* "PHL's Exoplanets Catalog". UPR Arecibo. 2018-03-02. http://phl.upr.edu/projects/habitable-exoplanets-catalog/data/database.
* Onsi Fakhouri. "Exoplanet Orbit Database". Exoplanets.org. http://exoplanets.org/.
* "NASA Exoplanet Archive". Caltech. https://exoplanetarchive.ipac.caltech.edu/index.html.
* "Stars Within 20 Light Years". Atlas of the Universe. http://www.atlasoftheuniverse.com/20lys.html.

* v
* t
* e

Exoplanet search projects

* Exoplanetology
* Exoplanet

Ground-based|

* AAPS
* APF
* CORALIE
* EAPSNet
* ELODIE
* EPICS
* ESPRESSO
* FINDS Exo-Earths
* Geneva
* HARPS
* HARPS-N
* GPI
* HATNet
* HEK
* HiCIAO
* HIRES
* KELT
* LCES
* Magellan
* MARVELS
* MASCARA
* MEarth
* MicroFUN
* MINERVA
* Australis
* MOA
* N2K
* NGTS
* NESSI
* OGLE
* OPSP
* PlanetPol
* Project 1640
* PARAS
* SEEDS
* SETI
* SOPHIE
* SPECULOOS
* SPHERE
* SuperWASP
* Systemic
* TrES
* XO Telescope
* ZIMPOL/CHEOPS

Space missions|

| Past|

* MOST (2003–2019)
* SWEEPS using HST (2006)
* CoRoT (2006–2013)
* EPOXI using Deep Impact (2008–2013)
* Kepler (2009–2018)
* detected exoplanets

|

Current|

* Gaia (2013–present)
* ASTERIA (2017–present)
* TESS (2018–present)

Planned|

* CHEOPS (2019)
* James Webb Space Telescope (2021)
* PLATO (2026)
* ARIEL (2028)
* WFIRST (mid-2020s)

Proposed|

* ATLAST
* EXCEDE
* HabEx
* HDST
* LUVOIR
* Nautilus Deep Space Observatory
* New Worlds Mission
* OST
* PEGASE

Cancelled|

* Darwin
* EChO
* Eddington
* Space Interferometry Mission
* Terrestrial Planet Finder

* Detection methods
* Discoveries of exoplanets
* Lists of exoplanets
* nearest

* v
* t
* e

Exoplanetology

* Planet
* Definition
* IAU
* Planetary science

Main topics|

* Exoplanet
* Methods of detecting exoplanets
* Planetary system

Sizes
and types|

| Terrestrial|

* Carbon planet
* Coreless planet
* Desert planet
* Dwarf planet
* Ice planet
* Iron planet
* Lava planet
* Mega-Earth
* Ocean planet
* Sub-Earth
* Super-Earth

|

Gaseous|

* Eccentric Jupiter
* Gas dwarf
* Helium planet
* Hot Jupiter
* Hot Neptune
* Ice giant
* Mini-Neptune
* Super-Neptune
* Super-Jupiter

Other types|

* Brown dwarf
* Chthonian planet
* Circumbinary planet
* Disrupted planet
* Double planet
* Eyeball planet
* Mesoplanet
* Planemo
* Planet/Brown dwarf boundary
* Planetesimal
* Protoplanet
* Pulsar planet
* Sub-brown dwarf
* Ultra-cool dwarf
* Ultra-short period planets (USP)

Formation
and evolution|

* Accretion
* Accretion disk
* Asteroid belt
* Circumplanetary disk
* Circumstellar disc
* Circumstellar envelope
* Cosmic dust
* Debris disk
* Detached object
* Disrupted planet
* Excretion disk
* Exoplanetary Circumstellar Environments and Disk Explorer
* Exozodiacal dust
* Extraterrestrial materials
* Extraterrestrial sample curation
* Giant-impact hypothesis
* Gravitational collapse
* Hills cloud
* Interplanetary dust cloud
* Interplanetary medium
* Interplanetary space
* Interstellar cloud
* Interstellar dust
* Interstellar medium
* Interstellar space
* Kuiper belt
* List of interstellar and circumstellar molecules
* Merging stars
* Molecular cloud
* Nebular hypothesis
* Oort cloud
* Outer space
* Planetary migration
* Planetary system
* Planetesimal
* Planet formation
* Protoplanetary disk
* Ring system
* Rubble pile
* Sample-return mission
* Scattered disc
* Star formation

Systems|

* Exocomet
* Exomoon
* Interstellar comet
* Mean-motion resonances
* Retrograde planet
* Rogue planet
* Tidally detached exomoon
* Titius–Bode laws
* Trojan planet

Host stars|

* A
* B
* Binary star
* Brown dwarfs
* Extragalactic planet
* F/Yellow-white dwarfs
* G/Yellow dwarfs
* Herbig Ae/Be
* K/Orange dwarfs
* M/Red dwarfs
* Planets in globular clusters
* Pulsar
* Red giant
* Subdwarf B
* Subgiant
* T Tauri
* White dwarfs
* Yellow giants

Detection|

* Astrometry
* Direct imaging
* list
* Microlensing
* list
* Polarimetry
* Pulsar timing
* list
* Radial velocity
* list
* Transit method
* list
* Transit-timing variation

Habitability|

* Astrobiology
* Circumstellar habitable zone
* Earth analog
* Extraterrestrial liquid water
* Habitability of natural satellites
* Superhabitable planet

Catalogues|

* Catalog of Nearby Habitable Systems
* Exoplanet Data Explorer
* Extrasolar Planets Encyclopaedia
* NASA Exoplanet Archive
* NASA Star and Exoplanet Database

Lists|

* Exoplanetary systems
* Host stars
* Multiplanetary systems
* Stars with proplyds
* Exoplanets
* Lists of exoplanets
* Discoveries
* Extremes
* Firsts
* Nearest
* Largest
* Most massive
* Terrestrial candidates
* Kepler
* Potentially habitable
* Discovered exoplanets by year
* before 2000
* 2000–2009
* 2010
* 2011
* 2012
* 2013
* 2014
* 2015
* 2016
* 2017
* 2018
* 2019

Other|

* Carl Sagan Institute
* Exoplanet phase curves
* Nexus for Exoplanet System Science
* Planets in science fiction
* Sudarsky's gas giant classification

* Discoveries of exoplanets
* Search projects

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