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List of nearest exoplanets

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Fomalhaut b (Dagon), 25 light-years away, with its parent star Fomalhaut blacked out, as pictured by Hubble in 2012. In 2020 this object was determined to be an expanding debris cloud from a collision of asteroids rather than a planet.
Distribution of nearest known exoplanets as of March 2018

There are 7,026 known exoplanets, or planets outside the Solar System that orbit a star, as of July 24, 2024; only a small fraction of these are located in the vicinity of the Solar System. Within 10 parsecs (32.6 light-years), there are 104 exoplanets listed as confirmed by the NASA Exoplanet Archive. Among the over 500 known stars and brown dwarfs within 10 parsecs, around 60 have been confirmed to have planetary systems; 51 stars in this range are visible to the naked eye, 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 2023 are two around Gliese 367 (30.7 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, and Proxima Centauri 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. 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, while planets named in the 2022 event include those around Gliese 436, Gliese 486, and Gliese 367.

Exoplanets within 10 parsecs

Key to colors
Mercury, Earth and Jupiter (for comparison purposes)
Confirmed multiplanetary systems
Exoplanets believed to be potentially habitable
Confirmed exoplanets
Host star system Companion exoplanet (in order from star) Notes and additional planetary observations
Name Distance
(ly)
Apparent
magnitude
(V) 		Mass
(M☉)
Label
 Mass
(ME)
 		Radius
(R🜨)
Semi-major axis
(AU)
Orbital period
(days)
Eccentricity
Inclination
(Β°)
Discovery
method 		Discovery year
Sun 0.000016 βˆ’26.7 1 Mercury 0.055 0.3829 0.387 88.0 0.205 β€” β€” β€” β€”
Earth 1 1 1 365.3 0.0167 β€” β€” β€”
Jupiter 317.8 10.973 5.20 4,333 0.0488 β€” β€” β€”
Proxima Centauri 4.2465 11.13 0.123 d β‰₯0.26 β€” 0.0289 5.122 0.04 β€” RV 2022 one disputed candidate (c)
b β‰₯1.07 β€” 0.0486 11.19 0.02 β€” RV 2016
Lalande 21185 8.304 7.52 0.46 b β‰₯2.69 β€” 0.0788 12.94 0.06 β€” RV 2019 1 candidate
c β‰₯13.6 β€” 2.94 2,946 0.13 β€” RV 2021
Epsilon Eridani 10.489 3.73 0.781 Γ†gir 242 β€” 3.53 2,689 0.26 166.5 RV 2000 1 inferred planet, 1 or possibly 2 inner debris discs, and an outer disc
Lacaille 9352 10.724 7.34 0.489 b β‰₯4.2 β€” 0.068 9.262 0.03 β€” RV 2019 1 candidate
c β‰₯7.6 β€” 0.120 21.79 0.03 β€” RV 2019
Ross 128 11.007 11.1 0.168 b β‰₯1.40 β€” 0.0496 9.866 0.12 β€” RV 2017
Groombridge 34 A 11.619 8.1 0.38 b β‰₯3.03 β€” 0.072 11.44 0.09 ~54? RV 2014
c β‰₯36 β€” 5.4 7,600 0.27 ~54? RV 2018
Epsilon Indi A 11.867 4.83 0.762 b 941 β€” 11.08 15,700 0.42 98.7 RV 2018
Tau Ceti 11.912 3.50 0.78 g β‰₯1.75 β€” 0.133 20.0 0.06 ~35? RV 2017 4 candidates
h β‰₯1.8 β€” 0.243 49.4 0.23 ~35? RV 2017
e β‰₯3.9 β€” 0.538 163 0.18 ~35? RV 2017
f β‰₯3.9 β€” 1.33 640 0.16 ~35? RV 2017
GJ 1061 11.984 7.52 0.113 b β‰₯1.4 β€” 0.021 3.20 <0.31 β€” RV 2019 two solutions for d's orbit
c β‰₯1.7 β€” 0.035 6.69 <0.29 β€” RV 2019
d β‰₯1.6 β€” 0.052 12.4 <0.54 β€” RV 2019
YZ Ceti 12.122 12.1 0.130 b β‰₯0.75 β€” 0.0156 1.97 0.0 β€” RV 2017 1 candidate
c β‰₯1.2 β€” 0.0209 3.06 0.04 β€” RV 2017
d β‰₯1.1 β€” 0.0276 4.66 0.03 β€” RV 2017
Luyten's Star 12.348 11.94 0.29 c β‰₯1.2 β€” 0.0365 4.72 0.12 β€” RV 2017
b β‰₯2.2 β€” 0.090 18.6 0.03 β€” RV 2017
d β‰₯10.8 β€” 0.712 414 0.17 β€” RV 2019
e β‰₯9.3 β€” 0.849 542 0.03 β€” RV 2019
Teegarden's Star 12.497 15.40 0.08 b β‰₯1.1 β€” 0.0252 4.91 0 β€” RV 2019
c β‰₯1.1 β€” 0.0443 11.4 0 β€” RV 2019
Wolf 1061 14.050 10.1 0.25 b β‰₯1.9 β€” 0.0375 4.89 0.03 β€” RV 2015
c β‰₯3.6 β€” 0.0890 17.9 0.03 β€” RV 2015
d β‰₯6.5 β€” 0.421 184 0.02 β€” RV 2015
TZ Arietis 14.578 12.30 0.14 b β‰₯67 β€” 0.88 771 0.46 β€” RV 2019 2 dubious candidates
Gliese 687 14.839 9.15 0.41 b β‰₯17.2 β€” 0.163 38.1 0.17 β€” RV 2014
c β‰₯16.0 β€” 1.165 728 0.40 β€” RV 2019
Gliese 674 14.849 9.38 0.35 b β‰₯11.2 β€” 0.039 4.69 0.23 β€” RV 2007
Gliese 876 15.238 10.2 0.33 d 6.8 β€” 0.0208 1.94 0.12 59.5 RV 2005
c 230 β€” 0.133 30.2 0.001 59.5 RV 2000
b 720 β€” 0.213 61.0 0.001 59.5 RV 1998
e 15 β€” 0.342 125 0.18 59.5 RV 2010
GJ 1002 15.806 13.84 0.12 b β‰₯1.08 β€” 0.0457 10.3 β€” β€” RV 2022
c β‰₯1.36 β€” 0.0738 21.2 β€” β€” RV 2022
Gliese 832 16.200 8.67 0.45 b β‰₯206 β€” 3.67 3,830 0.06 β€” RV 2008 1 disputed candidate
GJ 3323 17.531 12.2 0.164 b β‰₯2.0 β€” 0.0328 5.36 0.2 β€” RV 2017
c β‰₯2.3 β€” 0.126 40.5 0.2 β€” RV 2017
Gliese 251 18.215 9.65 0.372 b β‰₯4.0 β€” 0.0818 14.2 0.10 β€” RV 2020
Gliese 229 A 18.791 8.14 0.58 c β‰₯7.3 β€” 0.339 122 0.19 β€” RV 2020 Ab not confirmed until 2020.
b β‰₯8.5 β€” 0.898 526 0.10 β€” RV 2014
Gliese 752 A 19.292 9.13 0.46 b β‰₯13.6 β€” 0.338 106 0.03 β€” RV 2018
82 G. Eridani 19.704 4.26 0.85 b β‰₯2.7 β€” 0.121 18.3 ~0 β€” RV 2011 2 candidates
c β‰₯2.4 β€” 0.204 40.1 ~0 β€” RV 2011
d β‰₯4.8 β€” 0.350 90 ~0 β€” RV 2011
e β‰₯4.8 β€” 0.509 147 0.29 β€” RV 2017
EQ Pegasi A 20.400 10.38 0.436 b 718 β€” 0.643 284 0.35 69.2 Astrometry 2022
Gliese 581 20.549 10.5 0.31 e β‰₯1.7 β€” 0.0282 3.15 0.0 ~45? RV 2009 2 disputed candidates and a disc
b β‰₯16 β€” 0.0406 5.37 0.0 ~45? RV 2005
c β‰₯5.5 β€” 0.072 12.9 0.0 ~45? RV 2007
Gliese 338 B 20.658 7.0 0.64 b β‰₯10.3 β€” 0.141 24.5 0.11 β€” RV 2020
Gliese 625 21.131 10.2 0.30 b β‰₯2.8 β€” 0.0784 14.6 ~0.1 β€” RV 2017
HD 219134 21.336 5.57 0.78 b 4.7 1.60 0.0388 3.09 ~0 85.05 RV 2015
c 4.4 1.51 0.065 6.77 0.062 87.28 RV 2015
d β‰₯16 β€” 0.237 46.9 0.138 ~87? RV 2015
f β‰₯7.3 β€” 0.146 22.7 0.148 ~87? RV 2015
g β‰₯11 β€” 0.375 94.2 0 ~87? RV 2015
h (e) β‰₯108 β€” 3.11 2,247 0.06 ~87? RV 2015
LTT 1445 A 22.387 10.53 0.26 c 1.54 1.15 0.0266 3.12 <0.22 87.43 Transit 2021
b 2.87 1.30 0.0381 5.36 <0.11 89.68 Transit 2019
Gliese 393 22.953 8.65 0.41 b β‰₯1.71 β€” 0.0540 7.03 0.00 β€” RV 2019
Gliese 667 C 23.623 10.2 0.33 b β‰₯5.4 β€” 0.049 7.20 0.13 ~52? RV 2009 5 dubious candidates
c β‰₯3.9 β€” 0.1251 28.2 0.03 ~52? RV 2011
Gliese 514 24.878 9.03 0.53 b β‰₯5.2 β€” 0.421 140 0.45 β€” RV 2022
Gliese 486 26.351 11.395 0.32 b 2.8 1.31 0.0173 1.47 <0.05 88.4 Transit 2021
Gliese 686 26.613 9.58 0.42 b β‰₯7.1 β€” 0.097 15.5 0.04 β€” RV 2019
61 Virginis 27.836 4.74 0.95 b β‰₯5.1 β€” 0.0502 4.22 ~0.1 ~77? RV 2009 a debris disc, 1 disputed candidate
c β‰₯18 β€” 0.218 38.0 0.14 ~77? RV 2009
CD Ceti 28.052 14.001 0.161 b β‰₯3.95 β€” 0.0185 2.29 0 β€” RV 2020
Gliese 785 28.739 6.13 0.78 b β‰₯17 β€” 0.32 75 0.13 β€” RV 2010
c β‰₯24 β€” 1.18 530 ~0.3 β€” RV 2011
Gliese 849 28.750 10.4 0.49 b β‰₯270 β€” 2.26 1,910 0.05 β€” RV 2006
c β‰₯300 β€” 4.82 5,520 0.087 β€” RV 2006
Gliese 433 29.605 9.79 0.48 b β‰₯6.0 β€” 0.062 7.37 0.04 β€” RV 2009
d β‰₯5.2 β€” 0.178 36.1 0.07 β€” RV 2020
c β‰₯32 β€” 4.82 5,090 0.12 β€” RV 2012
HD 102365 A 30.396 4.89 0.85 b β‰₯16 β€” 0.46 122 0.34 β€” RV 2010
Gliese 367 30.719 9.98 0.45 b 0.55 0.72 0.0071 0.32 0 80.75 Transit 2021
Gliese 357 30.776 10.9 0.34 b 6.1 1.17 0.035 3.93 0.02 88.92 Transit 2019
c β‰₯3.6 β€” 0.061 9.13 0.04 ~89? RV 2019
d β‰₯7.7 β€” 0.204 55.7 0.03 ~89? RV 2019
Gliese 176 30.937 10.1 0.45 b β‰₯8.0 β€” 0.066 8.77 0.08 β€” RV 2007 1 disputed candidate
GJ 3512 30.976 13.11 0.123 b β‰₯147 β€” 0.338 204 0.44 β€” RV 2019
c β‰₯54 β€” >1.2 >1390 β€” β€” RV 2019
Wolf 1069 31.229 13.99 0.167 b β‰₯1.26 β€” 0.0672 15.6 β€” β€” RV 2023
AU Microscopii 31.683 8.63 0.50 b 17 4.38 0.0645 8.463 0.10 89.03 Transit 2020
c <28 3.51 0.1101 18.86 0 88.62 Transit 2020
Gliese 436 31.882 10.67 0.41 b 21.4 4.33 0.0280 2.64 0.15 85.8 RV 2004
Gliese 49 32.158 8.9 0.57 b β‰₯16.4 β€” 0.106 17.3 0.03 β€” RV 2019
HD 260655 32.608 9.77 0.439 b 2.14 1.240 0.0293 2.780 0.039 87.35 Transit 2022
c 3.09 1.533 0.0475 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. 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), LHS 288 (15.8 ly, in 2007), Gliese 682 (16.3 ly, in 2014), 40 Eridani A (16.3 ly, in 2018), and GJ 1151 (26.2 ly, in 2021). There are also several instances where proposed exoplanets were later disproved by subsequent studies, including candidates around Alpha Centauri B (4.36 ly), Barnard's Star (5.96 ly), Kapteyn's Star (12.8 ly), Van Maanen 2 (14.1 ly), Groombridge 1618 (15.9 ly), AD Leonis (16.2 ly), VB 10 (19.3 ly), and Fomalhaut (25.1 ly).

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

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. 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), SDSS J1416+1348 B (30.3 ly), and WISE 1217+1626 B (30 ly).

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), UGPS 0722-05, (13.4 ly) WISE 1541βˆ’2250 (18.6 ly), and SIMP J01365663+0933473 (20.0 ly).

See also

Notes

  1. Listed values are primarily taken from NASA Exoplanet Archive, 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).
  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).
  4. The star Epsilon Eridani was named Ran (after RΓ‘n, the Norse goddess of the sea), and the planet Epsilon Eridani b was named AEgir (after Γ†gir, RΓ‘n's husband), while the planet Fomalhaut b was named Dagon (after Dagon, an ancient Syrian β€œfish god”).
  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.
  7. This system is referred to as TZ Arietis, GJ 83.1, GJ 9066, or L 1159-16.

References

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