List of nearest exoplanets

There are 5,943 known exoplanets, or planets outside the Solar System that orbit a star, as of April 17, 2025; 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.

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

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 (ME)[note 6]	Radius (R🜨)	Semi-major axis (AU)	Orbital period (days)	Eccentricity	Inclination (°)	Discovery method	Discovery year
Sun°	0.000016	−26.7	1	Mercury	0.055	0.3829	0.387	88.0	0.205	—	—	—	—
				Earth	1	1	1	365.3	0.0167	—	—	—
				Jupiter	317.8	10.973	5.20	4,333	0.0488	—	—	—
Proxima Centauri#	4.2465	11.13	0.123	d	≥0.26	—	0.0289	5.122	0.04	—	RV	2022	[13][14] one disputed candidate (c)[15][16][17][18]
				b↑	≥1.07	—	0.0486	11.19	0.02	—	RV	2016
Barnard's Star#	5.9629	9.51	0.162	d	≥0.26	—	0.0188	2.340	0.04	—	RV	2025	[19]
				b	≥0.30	—	0.0229	3.154	0.03	—	RV	2024
				c	≥0.34	—	0.0274	4.124	0.08	—	RV	2025
				e	≥0.19	—	0.0381	6.739	0.04	—	RV	2025
Lalande 21185#	8.304	7.52	0.46	b	≥2.69	—	0.0788	12.94	0.06	—	RV	2019	1 candidate[20]
				c	≥13.6	—	2.94	2,946	0.13	—	RV	2021
Epsilon Eridani	10.501	3.73	0.82	Ægir	311	—	3.53	2,670	0.06	41	RV	2000	[21] 1 inferred planet, 1 or possibly 2 inner debris discs, and an outer disc[22]
Lacaille 9352#	10.724	7.34	0.489	b	≥4.2	—	0.068	9.262	0.03	—	RV	2019	1 candidate[23][24]
				c	≥7.6	—	0.120	21.79	0.03	—	RV	2019
Ross 128	11.007	11.1	0.168	b↑	≥1.40	—	0.0496	9.866	0.12	—	RV	2017	[25]
Gliese 725 A	11.491	8.94	0.330	b	≥2.78	—	0.068	11.2201	0.0	—	RV	2024	[26]
Groombridge 34 A#	11.619	8.1	0.38	b	≥3.03	—	0.072	11.44	0.09	~54?	RV	2014	[27][28]
				c	≥36	—	5.4	7,600	0.27	~54?	RV	2018
Epsilon Indi A	11.867	4.83	0.762	b	2005	—	28.4	63,400	0.40	103.7	RV	2018	nearest exoplanet directly imaged[29][30]
Tau Ceti#	11.912	3.50	0.78	g	≥1.75	—	0.133	20.0	0.06	~35?	RV	2017	4 disputed candidates [31][32][7][33][34][35]
				h	≥1.8	—	0.243	49.4	0.23	~35?	RV	2017
				e	≥3.9	—	0.538	163	0.18	~35?	RV	2017
				f	≥3.9	—	1.33	640	0.16	~35?	RV	2017
GJ 1061#	11.984	7.52	0.113	b	≥1.37	—	0.021	3.204	<0.31	—	RV	2019	two solutions for d's orbit[36]
				c↑	≥1.74	—	0.035	6.689	<0.29	—	RV	2019
				d↑	≥1.64	—	0.054	13.03	<0.53	—	RV	2019
YZ Ceti#	12.122	12.1	0.130	b	≥0.70	—	0.0163	2.021	0.06	—	RV	2017	[37]
				c	≥1.14	—	0.0216	3.060	0.0	—	RV	2017
				d	≥1.09	—	0.0285	4.656	0.07	—	RV	2017
Luyten's Star#	12.348	11.94	0.29	c	≥1.18	—	0.0365	4.723	0.10	—	RV	2017	2 candidates[38][23]
				b↑	≥2.89	—	0.0911	18.65	0.17	—	RV	2017
Teegarden's Star#	12.497	15.40	0.08	b↑	≥1.16	—	0.0259	4.906	0.03	—	RV	2019	[39][40]
				c↑	≥1.05	—	0.0455	11.42	0.04	—	RV	2019
				d	≥0.82	—	0.0791	26.13	0.07	—	RV	2024
Wolf 1061#	14.050	10.1	0.25	b	≥1.91	—	0.0375	4.887	0.15	—	RV	2015	[38]
				c↑	≥3.41	—	0.0890	17.87	0.11	—	RV	2015
				d	≥7.7	—	0.470	217	0.55	—	RV	2015
TZ Arietis	14.578	12.30	0.14	b	≥67	—	0.88	771	0.46	—	RV	2019	2 refuted candidates[23][41][42]
Gliese 687#	14.839	9.15	0.41	b	≥17.2	—	0.163	38.14	0.17	—	RV	2014	[23][41]
				c	≥16.0	—	1.165	728	0.40	—	RV	2019
Gliese 674	14.849	9.38	0.35	b	≥11.1	—	0.039	4.694	0.20	—	RV	2007	[43]
Gliese 876#	15.238	10.2	0.33	d	6.68	—	0.0210	1.938	0.04	56.7	RV	2005	[44]
				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	13.84	0.12	b↑	≥1.08	—	0.0457	10.35	—	—	RV	2022	[45]
				c↑	≥1.36	—	0.0738	21.2	—	—	RV	2022
Gliese 832	16.200	8.67	0.45	b	315	—	3.7	3,853	0.05	51 or 134	RV	2008	1 refuted candidate[46][47]
GJ 3323#	17.531	12.2	0.164	b	≥2.0	—	0.0328	5.36	0.2	—	RV	2017	[38]
				c	≥2.3	—	0.126	40.5	0.2	—	RV	2017
Gliese 251	18.215	9.65	0.372	b	≥4.0	—	0.0818	14.2	0.10	—	RV	2020	[48]
Gliese 752 A	19.292	9.13	0.46	b	≥12.2	—	0.343	106	0.10	—	RV	2018	[49][50]
82 G. Eridani#	19.704	4.26	0.79	b	≥2.15	—	0.126	18.3	0.06	—	RV	2011	[51]
				c	≥2.98	—	0.363	89.7	0.08	—	RV	2011
				d↑	≥5.82	—	1.354	648	0.45	—	RV	2023
HN Librae	20.395	11.32	0.29	b	≥5.5	—	0.142	36.1	0.08	—	RV	2023	1 candidate[52]
EQ Pegasi A	20.400	10.38	0.436	b	718	—	0.643	284	0.35	69.2	Astrometry	2022	[53]
Gliese 581#	20.549	10.5	0.295	e	2.5	—	0.0280	3.15	0.01	47	RV	2009	3 refuted candidates and a disc[54]
				b	20.5	—	0.0399	5.37	0.03	47	RV	2005
				c	6.8	—	0.0718	12.9	0.03	47	RV	2007
Gliese 338 B	20.658	7.0	0.64	b	≥10.3	—	0.141	24.5	0.11	—	RV	2020	[55]
Gliese 625	21.131	10.2	0.30	b	≥2.8	—	0.0784	14.6	~0.1	—	RV	2017	[56]
HD 219134#	21.336	5.57	0.78	b	4.7	1.60	0.0388	3.09	~0	85.05	RV	2015	[57][58][59]
				c	4.4	1.51	0.065	6.77	0.062	87.28	RV	2015
				f	≥7.3	—	0.146	22.7	0.148	~87?	RV	2015
				d	≥16	—	0.237	46.9	0.138	~87?	RV	2015
				g	≥11	—	0.375	94.2	0	~87?	RV	2015
				h (e)	≥108	—	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	1 candidate[60][61][62]
				b	2.87	1.30	0.0381	5.36	<0.11	89.68	Transit	2019
Gliese 393	22.953	8.65	0.41	b	≥1.71	—	0.0540	7.03	0.00	—	RV	2019	[23][63]
Gliese 667 C#	23.623	10.2	0.33	b	≥5.4	—	0.049	7.20	0.13	~52?	RV	2009	5 dubious candidates [64][7][65][66][23]
				c↑	≥3.9	—	0.1251	28.2	0.03	~52?	RV	2011
Gliese 514	24.878	9.03	0.53	b	≥5.2	—	0.421	140	0.45	—	RV	2022	[67]
GJ 1151	26.231	14.01	0.164	c	≥10.6	—	0.571	390	—	—	RV	2023	1 refuted candidate[68][69][70][71]
Gliese 486	26.351	11.395	0.32	Su	2.8	1.31	0.0173	1.47	<0.05	88.4	Transit	2021	[72]
Gliese 686	26.613	9.58	0.42	b	≥7.1	—	0.097	15.5	0.04	—	RV	2019	[73][23]
GJ 1289	27.275	12.67[74]	0.21	b	≥6.3	—	0.27	112	0	—	RV	2024	[75]
61 Virginis#	27.836	4.74	0.95	b	≥6.1	—	0.05	4.22	0.05	~77?	RV	2009	a debris disc[76]
				c	≥17.9	—	0.22	38.1	0.06	~77?	RV	2009
				d	≥10.5	—	0.47	123	0.12	~77?	RV	2009
CD Ceti	28.052	14.001	0.161	b	≥3.95	—	0.0185	2.29	0	—	RV	2020	[77]
Gliese 785#	28.739	6.13	0.78	b	≥17	—	0.32	75	0.13	—	RV	2010	[78]
				c	≥24	—	1.18	530	~0.3	—	RV	2011
Gliese 849#	28.750	10.4	0.49	b	≥270	—	2.26	1,910	0.05	—	RV	2006	[79][23]
				c	≥300	—	4.82	5,520	0.087	—	RV	2006
Gliese 433#	29.605	9.79	0.48	b	≥6.0	—	0.062	7.37	0.04	—	RV	2009	[80][23][81]
				d	≥5.2	—	0.178	36.1	0.07	—	RV	2020
				c	≥32	—	4.82	5,090	0.12	—	RV	2012
HD 102365 A	30.396	4.89	0.85	b	≥16	—	0.46	122	0.34	—	RV	2010	[82]
Gliese 367#	30.719	9.98	0.45	Tahay	0.63	0.70	0.0071	0.322	0.06	79.89	Transit	2021	[83][84]
				c	≥4.1	—	0.077	11.5	0.09	~80?	RV	2023
				d	≥6.0	—	0.159	34.4	0.14	~80?	RV	2023
Gliese 357#	30.776	10.9	0.34	b	6.1	1.17	0.035	3.93	0.02	88.92	Transit	2019	[85][23]
				c	≥3.6	—	0.061	9.13	0.04	~89?	RV	2019
				d↑	≥7.7	—	0.204	55.7	0.03	~89?	RV	2019
Gliese 176	30.937	10.1	0.45	b	≥8.0	—	0.066	8.77	0.08	—	RV	2007	1 disputed candidate[86][87][23]
GJ 3512#	30.976	15.1	0.123	b	≥147	—	0.338	204	0.44	—	RV	2019	[88][89]
				c	≥143	—	1.722	2,350	—	—	RV	2020
G 192-15#	31.075	14.5	0.132	b	≥1.03	—	0.0172	2.275	0	—	RV	2025	[89]
				c	≥14.3	—	1.137	1,219	0.68	—	RV	2025
Wolf 1069	31.229	13.99	0.167	b↑	≥1.26	—	0.0672	15.56	—	—	RV	2023	[90]
AU Microscopii#	31.683	8.63	0.50	b	17	4.38	0.0645	8.463	0.10	89.03	Transit	2020	2 candidates[91][92][93][94]
				c	<28	3.51	0.1101	18.86	0	88.62	Transit	2020
Gliese 436	31.882	10.67	0.41	Awohali	21.4	4.33	0.0280	2.64	0.15	85.8	RV	2004	[95][96]
G 268-110	31.888	14.5	0.137	b	≥1.52	—	0.0128	1.433	0	—	RV	2025	[89]
Gliese 49	32.158	8.9	0.57	b	≥16.4	—	0.106	17.3	0.03	—	RV	2019	[97]
GJ 3988	32.316	13.6	0.184	b	≥3.7	—	0.0405	6.944	0	—	RV	2023	[98]
HD 260655#	32.608	9.77	0.439	b	2.14	1.240	0.0293	2.780	0.039	87.35	Transit	2022	[99]
				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.^[100] 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),^[23] LHS 288 (15.8 ly, in 2007),^[101] and Gliese 682 (16.3 ly, in 2014).^[81] There are also several instances where proposed exoplanets were later disproved by subsequent studies, including candidates around Alpha Centauri B (4.36 ly),^[102] Kapteyn's Star (12.8 ly),^[103] Van Maanen 2 (14.1 ly),^[104] Groombridge 1618 (15.9 ly),^[105] AD Leonis (16.2 ly),^[106] 40 Eridani A (16.3 ly),^[107][108] Gliese 229 A (18.8 ly),^[109] VB 10 (19.3 ly),^[110] and Fomalhaut (25.1 ly).^[111]

In 2021, a candidate planet was detected around Vega, though it has yet to be confirmed.^[112] 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.^[113] Candidate planets around Luyten 726-8 (8.77 ly)^[114] and GJ 3378 (25.2 ly) were reported in 2024.^[75]

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.^[115] 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),^[116] SDSS J1416+1348 B (30.3 ly),^[117] and WISE 1217+1626 B (30 ly).^[118]

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),^[119] UGPS 0722-05, (13.4 ly)^[120] WISE 1541−2250 (18.6 ly),^[121] and SIMP J01365663+0933473 (20.0 ly).^[122]

See also

• List of nearest stars and brown dwarfs
• List of nearest bright stars
• List of nearest terrestrial exoplanet candidates
• Lists of planets
• List of planet types
• List of potentially habitable exoplanets
• Lists of astronomical objects

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.

   "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).^[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 (M_real*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]