Astronomy:List of nearest exoplanets

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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 2025 is a system around Barnard's Star (6.0 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]

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]
Lacaille 9352# 10.724 0734 7.34 rowspan="2"| 0.489 b 0004.2000 ≥4.2 — 0.068 9.262 0.03 — RV 2019 1 candidate[24][25]
c 0007.6000 ≥7.6 — 0.120 21.79 0.03 — RV 2019
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 [26]
Gliese 725 A 11.491 8.94 0.330 b ≥2.78 — 0.068 11.2201 0.0 — RV 2024 [27]
Gliese 725 B 11.491 9.70 0.25 c ≥3.4 — 0.139 37.90 — — RV 2025 [28]
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 [29][30]
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[31][32]
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[33]
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 [34]
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[35][24]
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 [36][37]
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 [35]
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[24][38][39]
Gliese 687# 14.839 0915 9.15 rowspan="2" |0.41 b 0017.2000 ≥17.2 — 0.163 38.14 0.17 — RV 2014 [24][38]
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 [40]
Gliese 876# 15.238 1020 10.2 rowspan = "4"|0.33 d 6.68 — 0.0210 1.938 0.04 56.7 RV 2005 [41]
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 [42]
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[43][44]
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 [35]
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 [45][46]
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 [47][48]
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 [49]
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[50]
EQ Pegasi A 20.400 1038 10.38 0.436 b 0718 718 — 0.643 0284.39 284 0.35 69.2 Astrometry 2022 [51]
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[52]
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 [53]
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 [54]
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 [55][56][57] Has 1 candidate planet (g)[58]
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[59][60][61]
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 [24][62]
Gliese 667 C# 23.623 1022 10.2 rowspan = "2"|0.33 b3 b 0005.4000 ≥5.4 — 0.049 00072 7.20 0.13 ~52? RV 2009 5 dubious candidates
[63][7][64][65][24]
c3 c

↑ || 0003.9000 ≥3.9

— 0.1251 0028 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 [66]
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 [67]
Gliese 686 26.613 0958 9.58 0.42 b 0007.1000 ≥7.1 — 0.097 0015.5 15.5 0.04 — RV 2019 [68][24]
GJ 1289 27.275 12.67[69] 0.21 b 0006.27 ≥6.3 — 0.27 112 0 — RV 2024 [70]
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[71]
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 [72]
Gliese 785# 28.739 0613 6.13 rowspan = "2"|0.78 b 0016.9000 ≥17 — 0.32 0074.7 75 0.13 — RV 2010 [73]
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 [74][24]
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 [75][24][76]
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 [77][78]
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 [79][24]
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[80][81][24]
GJ 3512# 30.976 1505 15.1 rowspan="2" | 0.123 b 0146.7000 ≥147 — 0.338 204 0.44 — RV 2019 [82][83]
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 [83]
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 [84]
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 [85] 2 candidates[86][87][88][89]
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 [90][91] One dubious candidate (UCF-1.01)[92]
G 268-110 31.888 1447 14.5 0.137 b 0001.5200 ≥1.52 — 0.0128 1.433 0 — RV 2025 [83]
Gliese 49 32.158 0890 8.9 0.57 b 0016.4000 ≥16.4 — 0.106 17.3 0.03 — RV 2019 [93]
GJ 3988 32.316 1363 13.6 0.184 b 0003.6900 ≥3.7 — 0.0405 6.944 0 — RV 2023 [94]
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 [95]
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.[96] 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),[24] Tau Ceti (11.9 ly, in 2012 & 2017),[97] Gliese 682 (16.3 ly, in 2014),[76] and HD 102365 A (30.4 ly, in 2011).[97] There are also several instances where proposed exoplanets were later disproved by subsequent studies, including candidates around Alpha Centauri B (4.36 ly),[98] Kapteyn's Star (12.8 ly),[99] Van Maanen 2 (14.1 ly),[100] Groombridge 1618 (15.9 ly),[101] AD Leonis (16.2 ly),[102] 40 Eridani A (16.3 ly),[103][104] Gliese 229 A (18.8 ly),[105] VB 10 (19.3 ly),[106] and Fomalhaut (25.1 ly).[107]

A candidate planet around LHS 288 was proposed in 2007, but it has not been confirmed.[108] In 2021, a candidate planet was detected around Vega, though it has yet to be confirmed.[109] 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.[110] 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.[111][70][112]

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.[113] 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),[114] SDSS J1416+1348 B (30.3 ly),[115] and WISE 1217+1626 B (30 ly).[116]

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),[117] UGPS 0722-05, (13.4 ly)[118] WISE 1541−2250 (18.6 ly),[119] and SIMP J01365663+0933473 (20.0 ly).[120]

See also

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]

References

  1. ↑ "NASA's Webb Images Cold Exoplanet 12 Light-Years Away". NASA Webb Mission Team. 24 July 2024. https://science.nasa.gov/missions/webb/nasas-webb-images-cold-exoplanet-12-light-years-away/. 
  2. ↑ Schneider, Jean (1995). "Interactive Extra-solar Planets Catalog". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/. Retrieved 2018-03-20. 
  3. ↑ 3.0 3.1 3.2 "NASA Exoplanet Archive—Confirmed Planetary Systems". California Institute of Technology. https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PSCompPars. 
  4. ↑ 4.0 4.1 Reylé, Céline; Jardine, Kevin; Fouqué, Pascal; Caballero, Jose A.; Smart, Richard L.; Sozzetti, Alessandro (30 April 2021). "The 10 parsec sample in the Gaia era". Astronomy & Astrophysics 650: A201. doi:10.1051/0004-6361/202140985. Bibcode: 2021A&A...650A.201R.  Data available at https://gruze.org/10pc/
  5. ↑ Bortle, John E. (2001). "Light Pollution And Astronomy: The Bortle Dark-Sky Scale". Sky & Telescope. http://www.skyandtelescope.com/resources/darksky/3304011.html. Retrieved 2014-05-20. 
  6. ↑ Powell, Richard (2006). "Stars within 50 light years". An Atlas of the Universe. http://www.atlasoftheuniverse.com/50lys.html. 
  7. ↑ 7.0 7.1 7.2 "The Habitable Exoplanets Catalog". University of Puerto Rico in Arecibo. 2015-09-01. http://phl.upr.edu/projects/habitable-exoplanets-catalog. 
  8. ↑ "epsilon Eridani". International Astronomical Union. http://nameexoworlds.iau.org/systems/105. 
  9. ↑ "Fomalhaut (alpha Piscis Austrini)". International Astronomical Union. http://nameexoworlds.iau.org/systems/103. 
  10. ↑ 10.0 10.1 "Final Results of NameExoWorlds Public Vote Released" (Press release). International Astronomical Union. 2015-12-15. Archived from the original on 2018-05-15. Retrieved 2018-03-17.
  11. ↑ "2022 Approved Names". IAU. https://www.nameexoworlds.iau.org/2022approved-names. 
  12. ↑ Cumming, Andrew; Butler, R. Paul; Marcy, Geoffrey W. et al. (2008). "The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets". Publications of the Astronomical Society of the Pacific 120 (867): 531–554. doi:10.1086/588487. Bibcode: 2008PASP..120..531C. 
  13. ↑ Anglada-Escudé, Guillem; Amado, Pedro J.; Barnes, John et al. (2016). "A terrestrial planet candidate in a temperate orbit around Proxima Centauri". Nature 536 (7617): 437–440. doi:10.1038/nature19106. PMID 27558064. Bibcode: 2016Natur.536..437A. https://www.nature.com/articles/nature19106. 
  14. ↑ Faria, J. P.; Suárez Mascareño, A. et al. (January 4, 2022). "A candidate short-period sub-Earth orbiting Proxima Centauri". Astronomy & Astrophysics (European Southern Observatory) 658: 17. doi:10.1051/0004-6361/202142337. Bibcode: 2022A&A...658A.115F. https://www.eso.org/public/archives/releases/sciencepapers/eso2202/eso2202a.pdf. 
  15. ↑ Suárez Mascareño, Alejandro et al. (29 July 2025). "Diving into the planetary system of Proxima with NIRPS: Breaking the metre per second barrier in the infrared". Astronomy & Astrophysics 700: A11. doi:10.1051/0004-6361/202553728. Bibcode: 2025A&A...700A..11S. 
  16. ↑ Damasso, Mario; Del Sordo, Fabio; Anglada-Escudé, Guillem et al. (15 January 2020). "A low-mass planet candidate orbiting Proxima Centauri at a distance of 1.5 AU". Science Advances 6 (3): eaax7467. doi:10.1126/sciadv.aax7467. PMID 31998838. Bibcode: 2020SciA....6.7467D. 
  17. ↑ Kervella, Pierre; Arenou, Frédéric; Schneider, Jean (2020). "Orbital inclination and mass of the exoplanet candidate Proxima c". Astronomy & Astrophysics 635: L14. doi:10.1051/0004-6361/202037551. ISSN 0004-6361. Bibcode: 2020A&A...635L..14K. 
  18. ↑ Benedict, G. Fritz; McArthur, Barbara E. (16 June 2020). "A Moving Target—Revising the Mass of Proxima Centauri c". Research Notes of the AAS 4 (6): 86. doi:10.3847/2515-5172/ab9ca9. Bibcode: 2020RNAAS...4...86B. 
  19. ↑ Artigau, Étienne; Cadieux, Charles; Cook, Neil J.; Doyon, René; Vandal, Thomas; Donati, Jean-Françcois; Moutou, Claire; Delfosse, Xavier et al. (2022). "Line-by-line Velocity Measurements: An Outlier-resistant Method for Precision Velocimetry". The Astronomical Journal 164 (3): 84. doi:10.3847/1538-3881/ac7ce6. Bibcode: 2022AJ....164...84A. 
  20. ↑ Basant, Ritvik et al. (March 2025). "Four Sub-Earth Planets Orbiting Barnard's Star from MAROON-X and ESPRESSO". The Astrophysical Journal Letters 982 (1): L1. doi:10.3847/2041-8213/adb8d5. Bibcode: 2025ApJ...982L...1B. 
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  103. ↑ 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. 
  104. ↑ 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. 
  105. ↑ 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. 
  106. ↑ "VB 10 b". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/vb_10_b--550/. Retrieved 2015-09-17. 
  107. ↑ 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. 
  108. ↑ . doi:10.1086/599044. Bibcode: 2009PASP..121..365B. 
  109. ↑ 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. 
  110. ↑ 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. 
  111. ↑ 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. 
  112. ↑ 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. 
  113. ↑ 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. 
  114. ↑ "SCR 1845 b". Extrasolar Planets Encyclopaedia. 2012-04-13. https://exoplanet.eu/catalog/scr_1845_b--321/. Retrieved 2015-09-17. 
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  117. ↑ 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/. 
  118. ↑ 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. 
  119. ↑ 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. 
  120. ↑ "Astronomers discover a nearby free-range planet with incredible magne". 3 August 2018. https://www.astronomy.com/news/2018/08/free-range-planet. 

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