List of nearest exoplanets

There are 4,414 known exoplanets, or planets outside the Solar System that orbit a star, as of February 1, 2021; only a small fraction of these are located in the vicinity of the Solar System.[3] Within 10 parsecs (32.6 light-years), there are 97 exoplanets listed as confirmed by the NASA Exoplanet Archive.[note 1][4] Among the over 400 known stars within 10 parsecs,[note 2][6] around 60 have been confirmed to have planetary systems; 51 stars in this range are visible to the naked eye,[note 3][8] nine of which have planetary systems.

Exoplanet Fomalhaut b (Dagon), 25 light-years away, with its parent star Fomalhaut blacked out, as pictured by Hubble in 2012.[1] In 2020 this object was determined to be an expanding debris cloud from a collision of asteroids rather than a planet.[2]
Distribution of nearest exoplanets

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 2020 is one around AU Microscopii (32 ly). The closest exoplanet found is Proxima Centauri b, which was confirmed in 2016 to orbit Proxima Centauri, the closest star to the Solar System (4.25 ly). 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 two planets (around YZ Ceti, 12 ly) which may be less massive than Earth. Several confirmed exoplanets are hypothesized to be potentially habitable, with Proxima Centauri b and Gliese 667 Cc (23.6 ly) considered among the most likely candidates.[9] The International Astronomical Union took a public survey in 2015 to assign proper names to some known extrasolar bodies, including the planets around Epsilon Eridani (10.5 ly) and Fomalhaut.[note 4][12]

Exoplanets within 10 parsecs
Key to colors
° Mercury, Earth and Jupiter (for comparison purposes)
# Confirmed multiplanetary systems
↑ Exoplanets believed to be potentially habitable[9]
Confirmed exoplanets[4]
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° 0−26.71 Mercury0.0550.38290.38788.0 0.205——— —
Earth111365.30.0167———
Jupiter317.810.9735.204,3330.0488———
Proxima Centauri# 4.244111.130.123 b↑>1.2~1.1?0.048611.20.109~133?RV2016 [14][9][15][16][17] 1 candidate[18]
c7—1.4891,9280.04133RV2020
Barnard's Star 5.9589.5110.144 b>4.2—0.4302320.04—RV2018 [19][20]
Wolf 359# 7.89513.540.09 c>3.8—0.0182.690.15—RV2019 [20]
b>43.9—1.8452,9400.04—RV2019
Lalande 21185 8.3077.520.46 b>2.7—0.078912.90.12—RV2017 [20][21]
Epsilon Eridani 10.4893.730.781 Ægir248—3.482,6920.0789RV2000 1 inferred planet, 1 or possibly 2 inner debris discs, and an outer disc[22][23][24]
Lacaille 9352# 10.7217.340.489 b>4.2—0.0689.260.03—RV2019 1 candidate[20][25]
c>7.6—0.12021.80.03—RV2019
Ross 128 11.00711.10.168 b↑>1.4~1.2?0.04969.870.12—RV2017 [26]
Struve 2398 B# 11.4909.70.248 b>15.7—0.26191.30.06—RV2019 [20]
c>13.1—0.4281920.03—RV2019
Groombridge 34 A# 11.6188.10.38 b>3.03—0.07211.40.094~61?RV2014 [27][28][29]
c>36—5.47,6000.27~61?RV2018
Tau Ceti# 11.7533.500.78 g>1.7—0.13320.00.06—RV2017 4 candidates
[30][31][9][32][33][34]
h>1.8—0.24349.40.23—RV2017
e>3.9~1.6?0.5381630.18—RV2017
f↑>3.9—1.336400.16—RV2017
Epsilon Indi A 11.8694.830.762 b1030—11.5516,5000.2664.25RV2018 [35]

[36][37]

Gliese 1061# 11.9807.520.113 b>1.4—0.0213.20<0.31—RV2019 two solutions for d's orbit[38]
c↑>1.7—0.0356.69<0.29—RV2019
d↑>1.6—0.05212.4<0.54—RV2019
YZ Ceti# 12.10812.10.130 b>0.75—0.01561.970.0—RV2017 1 candidate
[39][40][20]
c>1.2—0.02093.060.04—RV2017
d>1.1—0.02764.660.03—RV2017
Luyten's Star# 12.19911.940.29 c>1.2—0.03654.720.12—RV2017 [9][41][20]
b↑>2.2~1.4?0.09018.60.03—RV2017
d>10.8—0.7124140.17—RV2019
e>9.3—0.8495420.03—RV2019
Teegarden's Star# 12.49615.400.08 b↑>1.1—0.02524.910—RV2019 [42]
c↑>1.1—0.044311.40—RV2019
Kapteyn's Star# 12.8298.80.28 c>6.9—0.3111210.07—RV2014 [43] 1 disputed candidate[44][20]
Wolf 1061# 14.04610.10.25 b>1.9—0.03754.890.03—RV2015 [9][45][20]
c↑>3.6~1.5?0.0890 17.90.03—RV2015
d>6.5—0.4211840.02—RV2015
Gliese 83.1# 14.58412.300.14 b>30.9—0.4032420.18—RV2019 1 candidate[20][46][note 7]
c>71.6—0.8707680.33—RV2019
Gliese 674 14.8399.380.35 b>11.2—0.0394.690.23—RV2007 [47][48][20]
Gliese 687# 14.8409.150.41 b>17.2—0.16338.10.17—RV2014 [49][20][46]
c>16.0—1.1657280.40—RV2019
Gliese 876# 15.25010.20.33 d6.8—0.02081.940.1259.5RV2005 [50][20]
c230—0.13330.20.00159.5RV2000
b720—0.21361.00.00159.5RV1998
e15—0.3421250.1859.5RV2010
Gliese 832# 16.1948.670.45 c↑>5.4~1.7?0.16435.70.06—RV2014 [9][51][20]
b>206—3.673,8300.06—RV2008
40 Eridani A 16.3864.40.84 b>8.5—0.22442.40.04~72?RV2018 [52]
Gliese 3323# 17.53312.20.164 b>2.0~1.3?0.03285.360.2—RV2017 [53]
c>2.3—0.12640.50.2—RV2017
Gliese 251 18.2049.650.372 b>4.0—0.081814.20.10—RV2020 2 previous candidates; replaced by a single-planet solution[54][20][21]
Gliese 205# 18.5927.970.63 b>10.3—0.10916.90.11—RV2019 [20]
c>13.8—0.6892710.04—RV2019
Gliese 229 A# 18.7778.140.58 c↑>7.3—0.3391220.19—RV2020 Ab not confirmed until 2020.[55]
b>8.5—0.8985260.10—RV2014
Gliese 752 A 19.2869.130.46 b>13.6—0.3381060.03—RV2018 [56][20]
Gliese 754 19.28912.230.18 b>9.8—0.27778.40.03—RV2019 [20]
Gliese 588# 19.2989.310.46 b>2.4—0.0495.810.04—RV2019 [20]
c>10.3—0.5302060.06—RV2019
82 G. Eridani# 19.5824.260.85 b>2.7—0.12118.3~0—RV2011 2 candidates
[57][58][59]
c>2.4—0.20440.1~0—RV2011
d>4.8—0.35090~0—RV2011
e>4.8—0.509147 0.29—RV2017
Gliese 784 20.0837.970.5 b>9.4—0.0596.660.05—RV2019 [20]
Gliese 555 20.37011.320.29 b>30.1—0.7274500.04—RV2019 [20]
Gliese 581# 20.54510.50.31 e>1.7—0.02823.150.0~45?RV2009 2 disputed candidates and a disc
[60][61][62][63]
b>16—0.04065.370.0~45?RV2005
c>5.5—0.07212.90.0~45?RV2007
Gliese 338 B 20.6587.00.64 b>10.3—0.14124.50.11—RV2020 [64]
Gliese 625 21.11410.20.30 b>2.8—0.078414.6~0.1—RV2017 [65]
HD 219134# 21.3065.570.78 b4.71.600.03883.09~085.05RV2015 [66][67][68]
c4.41.510.0656.770.06287.28RV2015
d>16>1.610.23746.90.138~87?RV2015
f>7.3>1.310.14622.70.148~87?RV2015
g>11—0.37594.20~87?RV2015
h (e)>108—3.112,2470.06~87?RV2015
Gliese 880 22.3998.640.59 b↑>8.5—0.18739.40.13—RV2019 [20]
LTT 1445 A 22.40910.530.26 b~2.21.350.03815.360.1689.47Transit2019 [69]
Gliese 393 22.9388.650.41 b>1.9—0.0557.030.03—RV2019 [20]
Gliese 667 C# 23.63210.20.33 b>5.4—0.0497.200.13~52?RV2009 5 dubious candidates
[70][9][71][72][20]
c↑>3.9~1.5?0.125128.20.03~52?RV2011
Gliese 514 24.8519.030.53 b>4.3—0.09715.00.05—RV2019 [20]
Gliese 1151 26.23114.010.15 b>2.5—0.0172.020—Magnetic
interaction		2020 [73][74]
Gliese 300 26.46912.130.26 b↑>6.8—0.0508.330.29—RV2019 [20]
Gliese 686 26.6129.580.42 b>7.1—0.09715.50.04—RV2019 [75][20]
61 Virginis# 27.7414.740.95 b>5.1—0.05024.22~0.1~77?RV2009 a debris disc
[76]
c>18—0.21838.00.14~77?RV2009
d>23—0.4761230.35~77?RV2009
CD Ceti 28.08014.0010.161 b>4.0—0.01852.290—RV2020 [77]
Gliese 785# 28.6996.130.78 b>17—0.32750.13—RV2010 [78]
c>24—1.18530~0.3—RV2011
Gliese 849# 28.71110.40.49 b>270—2.261,9100.05—RV2006 [79][20]
c>300—4.82 5,5200.087—RV2006
Gliese 433# 29.5729.790.48 b>6.0—0.0627.370.04—RV2009 [80][20][55]
d>5.2—0.17836.10.07—RV2020
c>32—4.825,0900.12—RV2012
Gliese 3325 30.10911.730.27 b>11.8—0.07112.90.03—RV2019 [20]
HD 102365 A 30.3744.890.85 b>16—0.461220.34—RV2010 [81]
Gliese 357# 30.80310.90.34 b1.61.170.0353.930.0288.92Transit2019 [82][20]
c>3.6—0.0619.130.04~89?RV2019
d↑>7.7—0.20455.70.03~89?RV2019
Gliese 176# 30.87910.10.45 b>8.0—0.0668.770.08—RV2007 1 dubious planet[83][84][20]
c↑>7.4—0.14628.60.02—RV2019
Gliese 479 30.91210.660.43 b>5.1—0.07411.30.03—RV2019 [20]
Gliese 3512# 30.94913.110.123 b>147—0.3382040.44—RV2019 [85]
c>54—>1.2>1390——RV2019
AU Microscopii# 31.7198.630.50 b174.380.06458.4630.1089.03Transit2020 [86][87]
c<283.510.110118.86088.62Transit2020
Gliese 436 31.82010.670.41 b21.44.330.02802.640.1585.8RV2004 1 candidate[20]
Gliese 49 32.1458.90.57 b>16.4—0.10617.30.03—RV2019 [20]

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.[88] 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 LHS 288 (15.6 ly, in 2007[89]). There are also some instances where proposed exoplanets were later disproved by subsequent studies, including candidates around Alpha Centauri B (4.36 ly),[90] Van Maanen 2 (13.9 ly),[91] Groombridge 1618 (15.9 ly),[92] AD Leonis (16.2 ly),[93] Gliese 682 (16.6 ly),[55] VB 10 (18.7 ly),[94] and Fomalhaut (25.1 ly).[2]

In 2021, a candidate planet was detected around Vega, though it has yet to be confirmed.[95]

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.[96] Some proposed candidate exoplanets were later shown to be massive enough to fall above the threshold, and are likely brown dwarfs, as was the case for: SCR 1845-6357 B (12.6 ly),[97] SDSS J1416+1348 B (29.7 ly),[98] and WISE 1217+1626 B (30 ly).[99]

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 (7.3 ly),[100] UGPS 0722-05, (13 ly)[101] WISE 1541−2250 (18.6 ly),[102] and SIMP J01365663+0933473 (20 ly).[103]

Statistics

Planetary systems
Systems by planet count
Exoplanets No. of
systems		 Systems
6 1 HD 219134
5 0
4 4 Tau Ceti, Luyten's Star, Gliese 876, 82 G. Eridani
3 7 Gliese 1061, YZ Ceti, Wolf 1061, Gliese 581, 61 Virginis, Gliese 433, Gliese 357
2 19 —
1 28 —
Total 59
Distribution of nearby planet-hosting systems
Distance
(light-years)		 No. of known
star systems		 No. of known
stars		 No. of stars
hosting known
exoplanets		 Percentage of
stars hosting
exoplanets
< 5 1 3 1 33%
5–10 8 11 3 27%
10–15 31 43 16 37%
15–20 57 77 13 17%
20–25 55 78 11 14%
25–32.6 ? ~200 18 ~9%
Total >413[104] 62 <15.0%
Systems visible with
the naked eye?[note 3]
Visible host star? Systems
Yes (V < 6.5) 9
No (V > 6.5) 50

Exoplanets
Exoplanets by minimum estimated mass
Type Mass range[105] No.
Terran 0.5–5 M⊕ 46
Superterran 5–10 M⊕ 24
Neptunian 10–50 M⊕ 28
Jovian 50–600 M⊕ 10
Superjovian >600 M⊕ 3
Total 111
Exoplanets by orbital radius
Orbital radius No. Notes
< 0.4 AU 82 Mercury orbits at 0.39 AU
0.4–1.0 AU 16 Earth orbits at 1.0 AU
1.0–5 AU 11
> 5 AU 2 Jupiter orbits at 5.2 AU
Exoplanets by orbital period
Orbital period No. Notes
< 90 days 75 Mercury takes 88 days
90–365 days 17
1–10 years 14 Jupiter takes 11.9 years
> 10 years 5
Exoplanets by orbital eccentricity
Orbital eccentricity No. Notes
< 0.02 16 Earth's is 0.0167
0.02–0.20 78
Mercury's is 0.205
> 0.20 15
Exoplanets by discovery year
Year No.
1998 1
2000 2
2004 1
2005 2
2006 2
2007 3
2008 1
2009 6
2010 3
2011 5
2012 1
2014 5
2015 9
2016 1
2017 15
2018 5
2019 38
2020 9
2021 0

See also

Notes
  1. Listed values are primarily taken from NASA Exoplanet Archive,[4] 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". The Extrasolar Planets Encyclopaedia. Full table.
    "Exoplanets Data Explorer". Exoplanet Orbit Database. California Planet Survey. Click the "+" button to visualize additional parameters.
    "Open Exoplanet Catalogue". Click the "Show options" to visualize additional parameters. Archived from the original on 2017-09-02. Retrieved 2015-02-14.
  2. For reference, the 104th closest known star system in November 2016 was 82 Eridani (19.7 ly).[5]
  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).[7]
  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),[10] while the planet Fomalhaut b was named Dagon (after Dagon, an ancient Syrian “fish god”[11]).[12]
  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.[13]
  7. The star referred to as GJ 9066 in Feng et al. 2020 is the same as GJ 83.1 in Tuomi et al. 2019; see SIMBAD. Planets b and c are so called by Feng et al. 2020; in Tuomi et al. 2019 they are designated d and b, respectively. The planet designated c in Tuomi et al. 2019 was not detected by Feng et al. 2020, so it's considered a candidate here.

References
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  2. 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. arXiv:2004.08736. Bibcode:2020PNAS..117.9712G. doi:10.1073/pnas.1912506117. PMC 7211925. PMID 32312810. S2CID 215827666.
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  8. Powell, Richard (2006). "Stars within 50 light years". An Atlas of the Universe. Archived from the original on 2014-06-27. Retrieved 2014-05-17.
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  10. "epsilon Eridani". NameExoWorlds. International Astronomical Union. Archived from the original on 2018-02-15. Retrieved 2018-05-14.
  11. "Fomalhaut (alpha Piscis Austrini)". Nameexoworlds. International Astronomical Union. Archived from the original on 2017-04-30. Retrieved 2018-05-14.
  12. "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.
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  15. 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. Bibcode:2020SciA....6.7467D. doi:10.1126/sciadv.aax7467. PMC 6962037. PMID 31998838.
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