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List of nearest exoplanets
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There are 7,408 known exoplanets, or planets outside the Solar System that orbit a star, as of January 26, 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 106 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 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. 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 habitable12
Confirmed exoplanets13
Host star systemCompanion exoplanet (in order from star)Notes and additional planetary observations
NameDistance(ly) Apparentmagnitude (V)Mass(M☉) Label14Mass(ME)15Radius (R🜨) Semi-major axis(AU) Orbital period(days) Eccentricity Inclination(°) DiscoverymethodDiscovery year
Sun°0.000016−26.71Mercury0.0550.38290.38788.00.205————
Earth111365.30.0167———
Jupiter317.810.9735.204,3330.0488———
Proxima Centauri#4.246511.130.123d≥0.26—0.02895.1220.04—RV20221617 one disputed candidate (c)18192021
b↑≥1.07—0.048611.190.02—RV2016
Barnard's Star#5.96299.510.162d≥0.26—0.01882.3400.04—RV202522
b≥0.30—0.02293.1540.03—RV2024
c≥0.34—0.02744.1240.08—RV2025
e≥0.19—0.03816.7390.04—RV2025
Lalande 21185#8.3047.520.46b≥2.69—0.078812.940.06—RV20191 candidate23
c≥13.6—2.942,9460.13—RV2021
Epsilon Eridani10.5013.730.82Ægir311—3.532,6700.0641RV200024 1 inferred planet, 1 or possibly 2 inner debris discs, and an outer disc25
Lacaille 9352#10.7247.340.489b≥4.2—0.0689.2620.03—RV20191 candidate2627
c≥7.6—0.12021.790.03—RV2019
Ross 12811.00711.10.168b↑≥1.40—0.04969.8660.12—RV201728
Gliese 725 A11.4918.940.330b≥2.78—0.06811.22010.0—RV202429
Groombridge 34 A#11.6198.10.38b≥3.03—0.07211.440.09~54?RV20143031
c≥36—5.47,6000.27~54?RV2018
Epsilon Indi A11.8674.830.762b2005—28.463,4000.40103.7RV2018nearest exoplanet directly imaged3233
Tau Ceti#11.9123.500.78g≥1.75—0.13320.00.06~35?RV20174 disputed candidates343536373839
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
GJ 1061#11.9847.520.113b≥1.37—0.0213.204<0.31—RV2019two solutions for d's orbit40
c↑≥1.74—0.0356.689<0.29—RV2019
d↑≥1.64—0.05413.03<0.53—RV2019
YZ Ceti#12.12212.10.130b≥0.70—0.01632.0210.06—RV201741
c≥1.14—0.02163.0600.0—RV2017
d≥1.09—0.02854.6560.07—RV2017
Luyten's Star#12.34811.940.29c≥1.18—0.03654.7230.10—RV20172 candidates4243
b↑≥2.89—0.091118.650.17—RV2017
Teegarden's Star#12.49715.400.08b↑≥1.16—0.02594.9060.03—RV20194445
c↑≥1.05—0.045511.420.04—RV2019
d≥0.82—0.079126.130.07—RV2024
Wolf 1061#14.05010.10.25b≥1.91—0.03754.8870.15—RV201546
c↑≥3.41—0.089017.870.11—RV2015
d≥7.7—0.4702170.55—RV2015
TZ Arietis14.57812.300.14b≥67—0.887710.46—RV20192 refuted candidates474849
Gliese 687#14.8399.150.41b≥17.2—0.16338.140.17—RV20145051
c≥16.0—1.1657280.40—RV2019
Gliese 67414.8499.380.35b≥11.1—0.0394.6940.20—RV200752
Gliese 876#15.23810.20.33d6.68—0.02101.9380.0456.7RV200553
c235—0.130930.100.2656.7RV2000
b749—0.209861.100.0356.7RV1998
e16—0.3355123.60.0556.7RV2010
GJ 1002#15.80613.840.12b↑≥1.08—0.045710.35——RV202254
c↑≥1.36—0.073821.2——RV2022
Gliese 83216.2008.670.45b315—3.73,8530.0551 or 134RV20081 refuted candidate5556
GJ 3323#17.53112.20.164b≥2.0—0.03285.360.2—RV201757
c≥2.3—0.12640.50.2—RV2017
Gliese 25118.2159.650.372b≥4.0—0.081814.20.10—RV202058
Gliese 752 A19.2929.130.46b≥12.2—0.3431060.10—RV20185960
82 G. Eridani#19.7044.260.79b≥2.15—0.12618.30.06—RV201161
c≥2.98—0.36389.70.08—RV2011
d↑≥5.82—1.3546480.45—RV2023
HN Librae20.39511.320.29b≥5.5—0.14236.10.08—RV20231 candidate62
EQ Pegasi A20.40010.380.436b718—0.6432840.3569.2Astrometry202263
Gliese 581#20.54910.50.295e2.5—0.02803.150.0147RV20093 refuted candidates and a disc64
b20.5—0.03995.370.0347RV2005
c6.8—0.071812.90.0347RV2007
Gliese 338 B20.6587.00.64b≥10.3—0.14124.50.11—RV202065
Gliese 62521.13110.20.30b≥2.8—0.078414.6~0.1—RV201766
HD 219134#21.3365.570.78b4.71.600.03883.09~085.05RV2015676869
c4.41.510.0656.770.06287.28RV2015
f≥7.3—0.14622.70.148~87?RV2015
d≥16—0.23746.90.138~87?RV2015
g≥11—0.37594.20~87?RV2015
h (e)≥108—3.112,2470.06~87?RV2015
LTT 1445 A#22.38710.530.26c1.541.150.02663.12<0.2287.43Transit20211 candidate707172
b2.871.300.03815.36<0.1189.68Transit2019
Gliese 39322.9538.650.41b≥1.71—0.05407.030.00—RV20197374
Gliese 667 C#23.62310.20.33b≥5.4—0.0497.200.13~52?RV20095 dubious candidates7576777879
c↑≥3.9—0.125128.20.03~52?RV2011
Gliese 51424.8789.030.53b≥5.2—0.4211400.45—RV202280
GJ 115126.23114.010.164c≥10.6—0.571390——RV20231 refuted candidate81828384
Gliese 48626.35111.3950.32Su2.81.310.01731.47<0.0588.4Transit202185
Gliese 68626.6139.580.42b≥7.1—0.09715.50.04—RV20198687
GJ 128927.27512.67880.21b≥6.3—0.271120—RV202489
61 Virginis#27.8364.740.95b≥6.1—0.054.220.05~77?RV2009a debris disc90
c≥17.9—0.2238.10.06~77?RV2009
d≥10.5—0.471230.12~77?RV2009
CD Ceti28.05214.0010.161b≥3.95—0.01852.290—RV202091
Gliese 785#28.7396.130.78b≥17—0.32750.13—RV201092
c≥24—1.18530~0.3—RV2011
Gliese 849#28.75010.40.49b≥270—2.261,9100.05—RV20069394
c≥300—4.825,5200.087—RV2006
Gliese 433#29.6059.790.48b≥6.0—0.0627.370.04—RV2009959697
d≥5.2—0.17836.10.07—RV2020
c≥32—4.825,0900.12—RV2012
HD 102365 A30.3964.890.85b≥16—0.461220.34—RV201098
Gliese 367#30.7199.980.45Tahay0.630.700.00710.3220.0679.89Transit202199100
c≥4.1—0.07711.50.09~80?RV2023
d≥6.0—0.15934.40.14~80?RV2023
Gliese 357#30.77610.90.34b6.11.170.0353.930.0288.92Transit2019101102
c≥3.6—0.0619.130.04~89?RV2019
d↑≥7.7—0.20455.70.03~89?RV2019
Gliese 17630.93710.10.45b≥8.0—0.0668.770.08—RV20071 disputed candidate103104105
GJ 3512#30.97615.10.123b≥147—0.3382040.44—RV2019106107
c≥143—1.7222,350——RV2020
G 192-15#31.07514.50.132b≥1.03—0.01722.2750—RV2025108
c≥14.3—1.1371,2190.68—RV2025
Wolf 106931.22913.990.167b↑≥1.26—0.067215.56——RV2023109
AU Microscopii#31.6838.630.50b174.380.06458.4630.1089.03Transit20202 candidates110111112113
c<283.510.110118.86088.62Transit2020
Gliese 43631.88210.670.41Awohali21.44.330.02802.640.1585.8RV2004114115
G 268-11031.88814.50.137b≥1.52—0.01281.4330—RV2025116
Gliese 4932.1588.90.57b≥16.4—0.10617.30.03—RV2019117
GJ 398832.31613.60.184b≥3.7—0.04056.9440—RV2023118
HD 260655#32.6089.770.439b2.141.2400.02932.7800.03987.35Transit2022119
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.120 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),121 LHS 288 (15.8 ly, in 2007),122 and Gliese 682 (16.3 ly, in 2014).123 There are also several instances where proposed exoplanets were later disproved by subsequent studies, including candidates around Alpha Centauri B (4.36 ly),124 Kapteyn's Star (12.8 ly),125 Van Maanen 2 (14.1 ly),126 Groombridge 1618 (15.9 ly),127 AD Leonis (16.2 ly),128 40 Eridani A (16.3 ly),129130 Gliese 229 A (18.8 ly),131 VB 10 (19.3 ly),132 and Fomalhaut (25.1 ly).133

In 2021, a candidate planet was detected around Vega, though it has yet to be confirmed.134 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.135 Candidate planets around Luyten 726-8 (8.77 ly)136 and GJ 3378 (25.2 ly) were reported in 2024.137

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.138 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),139 SDSS J1416+1348 B (30.3 ly),140 and WISE 1217+1626 B (30 ly).141

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),142 UGPS 0722-05, (13.4 ly)143 WISE 1541−2250 (18.6 ly),144 and SIMP J01365663+0933473 (20.0 ly).145

See also

Notes

References

  1. Schneider, Jean (1995). "Interactive Extra-solar Planets Catalog". Extrasolar Planets Encyclopaedia. Archived from the original on 2012-02-12. Retrieved 2018-03-20. https://exoplanet.eu/catalog/ ↩

  2. 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. "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. /wiki/NASA_Exoplanet_Archive ↩

  3. "NASA Exoplanet Archive—Confirmed Planetary Systems". NASA Exoplanet Science Institute. California Institute of Technology. Retrieved 2023-08-18. https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PSCompPars ↩

  4. 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. arXiv:2104.14972. Bibcode:2021A&A...650A.201R. doi:10.1051/0004-6361/202140985. S2CID 233476431. Data available at https://gruze.org/10pc/ /wiki/Astronomy_%26_Astrophysics ↩

  5. For reference, the 100th closest known star system in April 2021 was EQ Pegasi (20.4 ly).[4] /wiki/EQ_Pegasi ↩

  6. 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] /wiki/Bortle_scale ↩

  7. 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. http://www.atlasoftheuniverse.com/50lys.html ↩

  8. "The Habitable Exoplanets Catalog". Planetary Habitability Laboratory. University of Puerto Rico in Arecibo. 2015-09-01. Archived from the original on 2016-01-09. Retrieved 2015-09-17. https://phl.upr.edu/projects/habitable-exoplanets-catalog ↩

  9. 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] /wiki/Epsilon_Eridani ↩

  10. "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. https://www.iau.org/news/pressreleases/detail/iau1514/ ↩

  11. "2022 Approved Names". nameexoworlds.iau.org. IAU. Retrieved 7 June 2023. https://www.nameexoworlds.iau.org/2022approved-names ↩

  12. "The Habitable Exoplanets Catalog". Planetary Habitability Laboratory. University of Puerto Rico in Arecibo. 2015-09-01. Archived from the original on 2016-01-09. Retrieved 2015-09-17. https://phl.upr.edu/projects/habitable-exoplanets-catalog ↩

  13. "NASA Exoplanet Archive—Confirmed Planetary Systems". NASA Exoplanet Science Institute. California Institute of Technology. Retrieved 2023-08-18. https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PSCompPars ↩

  14. 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. /wiki/Exoplanet_naming_convention ↩

  15. 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] /wiki/Radial_velocity ↩

  16. 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. arXiv:1609.03449. Bibcode:2016Natur.536..437A. doi:10.1038/nature19106. PMID 27558064. S2CID 4451513. https://www.nature.com/articles/nature19106 ↩

  17. Faria, J. P.; Suárez Mascareño, A.; et al. (January 4, 2022). "A candidate short-period sub-Earth orbiting Proxima Centauri" (PDF). Astronomy & Astrophysics. 658. European Southern Observatory: 17. arXiv:2202.05188. Bibcode:2022A&A...658A.115F. doi:10.1051/0004-6361/202142337. https://www.eso.org/public/archives/releases/sciencepapers/eso2202/eso2202a.pdf ↩

  18. 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. https://www.ncbi.nlm.nih.gov/pmc/articles/PMC6962037 ↩

  19. Kervella, Pierre; Arenou, Frédéric; Schneider, Jean (2020). "Orbital inclination and mass of the exoplanet candidate Proxima c". Astronomy & Astrophysics. 635: L14. arXiv:2003.13106. Bibcode:2020A&A...635L..14K. doi:10.1051/0004-6361/202037551. ISSN 0004-6361. S2CID 214713486. /wiki/ArXiv_(identifier) ↩

  20. 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. Bibcode:2020RNAAS...4...86B. doi:10.3847/2515-5172/ab9ca9. S2CID 225798015. https://doi.org/10.3847%2F2515-5172%2Fab9ca9 ↩

  21. Artigau, Étienne; Cadieux, Charles; Cook, Neil J.; Doyon, René; Vandal, Thomas; Donati, Jean-Françcois; Moutou, Claire; Delfosse, Xavier; Fouqué, Pascal; Martioli, Eder; Bouchy, François; Parsons, Jasmine; Carmona, Andres; Dumusque, Xavier; Astudillo-Defru, Nicola; Bonfils, Xavier; Mignon, Lucille (2022). "Line-by-line Velocity Measurements: An Outlier-resistant Method for Precision Velocimetry". The Astronomical Journal. 164 (3): 84. arXiv:2207.13524. Bibcode:2022AJ....164...84A. doi:10.3847/1538-3881/ac7ce6. S2CID 251105120. https://doi.org/10.3847%2F1538-3881%2Fac7ce6 ↩

  22. Basant, Ritvik; Luque, Rafael; et al. (March 2025). "Four Sub-Earth Planets Orbiting Barnard's Star from MAROON-X and ESPRESSO". The Astrophysical Journal Letters. 982 (1): L1. arXiv:2503.08095. Bibcode:2025ApJ...982L...1B. doi:10.3847/2041-8213/adb8d5. https://doi.org/10.3847%2F2041-8213%2Fadb8d5 ↩

  23. Hurt, Spencer A.; Fulton, Benjamin; Isaacson, Howard; Rosenthal, Lee J.; Howard, Andrew W.; Weiss, Lauren M.; Petigura, Erik A. (2021), "Confirmation of the Long-Period Planet Orbiting Gliese 411 and the Detection of a New Planet Candidate", The Astronomical Journal, 163 (5): 218, arXiv:2107.09087, Bibcode:2022AJ....163..218H, doi:10.3847/1538-3881/ac5c47, S2CID 236134034 /wiki/ArXiv_(identifier) ↩

  24. Thompson, William; Nielsen, Eric; Ruffio, Jean-Baptiste; Blunt, Sarah; Marois, Christian (2025-02-27). "Revised Mass and Orbit of $\varepsilon$ Eridani b: A 1 Jupiter-Mass Planet on a Near-Circular Orbit". arXiv.org. Retrieved 2025-03-03. https://arxiv.org/abs/2502.20561 ↩

  25. Booth, Mark; Pearce, Tim D; Krivov, Alexander V; Wyatt, Mark C; Dent, William R F; Hales, Antonio S; Lestrade, Jean-François; Cruz-Sáenz de Miera, Fernando; Faramaz, Virginie C; Löhne, Torsten; Chavez-Dagostino, Miguel (2023-03-30). "The clumpy structure of ϵ Eridani's debris disc revisited by ALMA". Monthly Notices of the Royal Astronomical Society. 521 (4). Oxford University Press (OUP): 6180–6194. arXiv:2303.13584. Bibcode:2023MNRAS.521.6180B. doi:10.1093/mnras/stad938. ISSN 0035-8711. https://doi.org/10.1093%2Fmnras%2Fstad938 ↩

  26. Barnes, J. R.; Kiraga, M.; Diaz, M.; Berdiñas, Z.; Jenkins, J. S.; Keiser, S.; Thompson, I.; Crane, J. D.; Shectman, S. A.; Teske, J. K.; Holden, B.; Laughlin, G.; Burt, J.; Vogt, S. S.; Arriagada, P.; Butler, R. P.; Anglada-Escudé, G.; Jones, H. R. A.; Tuomi, M. (11 June 2019). "Frequency of planets orbiting M dwarfs in the Solar neighbourhood". arXiv:1906.04644 [astro-ph.EP]. /wiki/ArXiv_(identifier) ↩

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