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There are 5,197 known exoplanets, or planets outside the Solar System that orbit a star, as of October 1, 2022; 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 500 known stars and brown dwarfs within 10 parsecs,[5][note 2] around 60 have been confirmed to have planetary systems; 51 stars in this range are visible to the naked eye,[note 3][7] eight of which have planetary systems.

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]
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 known exoplanets as of March 2018
Distribution of nearest known exoplanets as of March 2018

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 2022 is one around EQ Pegasi A (20 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 planets around YZ Ceti, Gliese 367, and Proxima Centauri 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.[8] 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][11] while planets that will be named in the 2022 event include those around Gliese 436, Gliese 486, and Gliese 367.[12]


Exoplanets within 10 parsecs


Key to colors
° Mercury, Earth and Jupiter (for comparison purposes)
# Confirmed multiplanetary systems
↑ Exoplanets believed to be potentially habitable[8]
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
(MEarth)[note 6]
 Radius
(REarth)
Semi-major axis
(AU)
Orbital period
(days)
Eccentricity
Inclination
(°)
Discovery
method		 Discovery year
Sun° 0.000016−26.71 Mercury0.0550.38290.38788.0 0.205——— —
Earth111365.30.0167———
Jupiter317.810.9735.204,3330.0488———
Proxima Centauri# 4.246511.130.123 d>0.26~0.81?0.028855.1220.04—RV2022 [14][8] one disputed candidate (c)[15][16][17][18]
b↑>1.2—0.048611.20.109—RV2016
Lalande 21185# 8.3047.520.46 b>2.7—0.078912.90.12—RV2019 [19][20][21][22][23]
c>24.7—3.103,1900.14—RV2021
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[24][25][26]
Lacaille 9352# 10.7247.340.489 b>4.2—0.0689.260.03—RV2019 1 candidate[19][27]
c>7.6—0.12021.80.03—RV2019
Ross 128 11.00711.10.168 b↑>1.4—0.04969.870.12—RV2017 [28]
Groombridge 34 A# 11.6198.10.38 b>3.03—0.07211.40.094~61?RV2014 [29][30][31]
c>36—5.47,6000.27~61?RV2018
Epsilon Indi A 11.8674.830.762 b1030—11.5516,5000.2664.25RV2018 [32][33][34]
Tau Ceti# 11.9123.500.78 g>1.75—0.13320.00.06~35?RV2017 4 candidates
[35][36][8][37][38][39]
h>1.8—0.24349.40.23~35?RV2017
e>3.9—0.5381630.18~35?RV2017
f>3.9—1.336400.16~35?RV2017
Gliese 1061# 11.9847.520.113 b>1.4—0.0213.20<0.31—RV2019 two solutions for d's orbit[40]
c↑>1.7—0.0356.69<0.29—RV2019
d↑>1.6—0.05212.4<0.54—RV2019
YZ Ceti# 12.12212.10.130 b>0.75—0.01561.970.0—RV2017 1 candidate
[41][42][19]
c>1.2—0.02093.060.04—RV2017
d>1.1—0.02764.660.03—RV2017
Luyten's Star# 12.34811.940.29 c>1.2—0.03654.720.12—RV2017 [8][43][19]
b↑>2.2—0.09018.60.03—RV2017
d>10.8—0.7124140.17—RV2019
e>9.3—0.8495420.03—RV2019
Teegarden's Star# 12.49715.400.08 b↑>1.1—0.02524.910—RV2019 [44]
c↑>1.1—0.044311.40—RV2019
Wolf 1061# 14.05010.10.25 b>1.9—0.03754.890.03—RV2015 [8][45][19]
c↑>3.6—0.0890 17.90.03—RV2015
d>6.5—0.4211840.02—RV2015
TZ Arietis 14.57812.300.14 b>67—0.887710.46—RV2019 2 dubious candidates[19][46][47][note 7]
Gliese 687# 14.8399.150.41 b>17.2—0.16338.10.17—RV2014 [48][19][46]
c>16.0—1.1657280.40—RV2019
Gliese 674 14.8499.380.35 b>11.2—0.0394.690.23—RV2007 [49][50][19]
Gliese 876# 15.23810.20.33 d6.8—0.02081.940.1259.5RV2005 [51][19]
c230—0.13330.20.00159.5RV2000
b720—0.21361.00.00159.5RV1998
e15—0.3421250.1859.5RV2010
Gliese 832 16.2008.670.45 b>206—3.673,8300.06—RV2008 1 disputed candidate[8][52][19][53]
Gliese 3323# 17.53112.20.164 b>2.0—0.03285.360.2—RV2017 [54]
c>2.3—0.12640.50.2—RV2017
Gliese 251 18.2159.650.372 b>4.0—0.081814.20.10—RV2020 2 previous candidates; replaced by a single-planet solution[55][19][20]
Gliese 229 A# 18.7918.140.58 c↑>7.3—0.3391220.19—RV2020 Ab not confirmed until 2020.[56]
b>8.5—0.8985260.10—RV2014
Gliese 752 A 19.2929.130.46 b>13.6—0.3381060.03—RV2018 [57][19]
82 G. Eridani# 19.7044.260.85 b>2.7—0.12118.3~0—RV2011 2 candidates
[58][59][60]
c>2.4—0.20440.1~0—RV2011
d>4.8—0.35090~0—RV2011
e>4.8—0.509147 0.29—RV2017
EQ Pegasi A 20.40010.380.436 b718—0.6432840.3569.2Astrometry2022 [61]
Gliese 581# 20.54910.50.31 e>1.7—0.02823.150.0~45?RV2009 2 disputed candidates and a disc
[62][63][64][65]
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 [66]
Gliese 625 21.13110.20.30 b>2.8—0.078414.6~0.1—RV2017 [67]
HD 219134# 21.3365.570.78 b4.71.600.03883.09~085.05RV2015 [68][69][70]
c4.41.510.0656.770.06287.28RV2015
d>16—0.23746.90.138~87?RV2015
f>7.3—0.14622.70.148~87?RV2015
g>11—0.37594.20~87?RV2015
h (e)>108—3.112,2470.06~87?RV2015
LTT 1445 A# 22.38710.530.26 c1.541.150.02663.12<0.2287.43Transit2021 [71][72]
b2.871.300.03815.36<0.1189.68Transit2019
Gliese 393 22.9538.650.41 b>1.71—0.05407.030.00—RV2019 [19][73]
Gliese 667 C# 23.62310.20.33 b>5.4—0.0497.200.13~52?RV2009 5 dubious candidates
[74][8][75][76][19]
c↑>3.9~1.5?0.125128.20.03~52?RV2011
Gliese 514 24.8789.030.53 b>5.2—0.4211400.45—RV2022 [77]
Gliese 486 26.35111.3950.32 b2.81.310.01731.47<0.0588.4Transit2021 [78]
Gliese 686 26.6139.580.42 b>7.1—0.09715.50.04—RV2019 [79][19]
61 Virginis# 27.8364.740.95 b>5.1—0.05024.22~0.1~77?RV2009 a debris disc,[80] 1 disputed candidate[22]
c>18—0.21838.00.14~77?RV2009
CD Ceti 28.05214.0010.161 b>3.95—0.01852.290—RV2020 [81]
Gliese 785# 28.7396.130.78 b>17—0.32750.13—RV2010 [82]
c>24—1.18530~0.3—RV2011
Gliese 849# 28.75010.40.49 b>270—2.261,9100.05—RV2006 [83][19]
c>300—4.82 5,5200.087—RV2006
Gliese 433# 29.6059.790.48 b>6.0—0.0627.370.04—RV2009 [84][19][56]
d>5.2—0.17836.10.07—RV2020
c>32—4.825,0900.12—RV2012
HD 102365 A 30.3964.890.85 b>16—0.461220.34—RV2010 [85]
Gliese 367 30.7199.980.45 b0.550.720.00710.32080.75Transit2021 [86]
Gliese 357# 30.77610.90.34 b6.11.170.0353.930.0288.92Transit2019 [87][19]
c>3.6—0.0619.130.04~89?RV2019
d↑>7.7—0.20455.70.03~89?RV2019
Gliese 176 30.93710.10.45 b>8.0—0.0668.770.08—RV2007 1 disputed candidate[88][89][19]
Gliese 3512# 30.97613.110.123 b>147—0.3382040.44—RV2019 [90]
c>54—>1.2>1390——RV2019
AU Microscopii# 31.6838.630.50 b174.380.06458.4630.1089.03Transit2020 [91][92]
c<283.510.110118.86088.62Transit2020
Gliese 436 31.88210.670.41 b21.44.330.02802.640.1585.8RV2004 1 candidate[93]
Gliese 49 32.1588.90.57 b>16.4—0.10617.30.03—RV2019 [94]
HD 260655# 32.6089.770.439 b2.141.2400.02932.7800.03987.35Transit2022 [95]
c3.091.5330.04755.7060.03887.79Transit2022

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),[19] LHS 288 (15.8 ly, in 2007),[97] 40 Eridani A (16.3 ly, in 2018),[98][22] and Gliese 1151 (26.2 ly, in 2021).[99][100][101] There are also several instances where proposed exoplanets were later disproved by subsequent studies, including candidates around Alpha Centauri B (4.36 ly),[102] Barnard's Star (5.96 ly),[103][104] Kapteyn's Star (12.8 ly),[105] Van Maanen 2 (14.1 ly),[106] Groombridge 1618 (15.9 ly),[107] AD Leonis (16.2 ly),[108] Gliese 682 (16.3 ly),[56] VB 10 (19.3 ly),[109] and Fomalhaut (25.1 ly).[2]

In 2021, a candidate planet was detected around Vega, though it has yet to be confirmed.[110] 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.[111]

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.[112] 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 (13.1 ly),[113] SDSS J1416+1348 B (30.3 ly),[114] and WISE 1217+1626 B (30 ly).[115]

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


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 100th closest known star system in April 2021 was EQ Pegasi (20.4 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).[6]
  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),[9] while the planet Fomalhaut b was named Dagon (after Dagon, an ancient Syrian “fish god”[10]).[11]
  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. This system is referred to as TZ Arietis, GJ 83.1, GJ 9066, or L 1159-16.

References


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