List of nearest exoplanets

There are known exoplanets, or planets outside the Solar System that orbit a star, as of ; only a small fraction of these are located in the vicinity of the Solar System. Within, 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, and the latest as of 2025 is a system around Barnard's Star. 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 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 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 and Fomalhaut, while planets named in the 2022 event include those around Gliese 436, Gliese 486, and Gliese 367.

Exoplanets within 10 parsecs

Host star system	Host star system	Host star system	Host star system	Companion exoplanet	Companion exoplanet	Companion exoplanet	Companion exoplanet	Companion exoplanet	Companion exoplanet	Companion exoplanet	Companion exoplanet	Companion exoplanet	Notes and additional planetary observations
Name	Distance	Apparent magnitude	Mass	Label	Mass	Radius	Semi-major axis	Orbital period	Eccentricity	Inclination	Discovery method	Discovery year	Notes and additional planetary observations
Sun^°	0.000016		1		'	0.3829	0.387	'	0.205	3.38	—		For comparison purposes. One candidate planet
Sun^°	0.000016		1		'	1	1	'	0.0167	7.25	—		For comparison purposes. One candidate planet
Sun^°	0.000016		1		'	'	5.20		0.0488	6.09	—		For comparison purposes. One candidate planet
Proxima Centauri^#	4.2465		0.123	d		~0.81 ± 0.08	0.0289	5.122	0.04	—	RV	2025	one disputed candidate
Proxima Centauri^#	4.2465		0.123	b^↑		0.94 – 1.4	0.0486	11.19	0.02	—	RV	2016	one disputed candidate
Barnard's Star^#	5.9629	9.51	0.162	d		—	0.0188	2.340	0.04	—	RV	2025
Barnard's Star^#	5.9629	9.51	0.162	b		—	0.0229	3.154	0.03	—	RV	2024
Barnard's Star^#	5.9629	9.51	0.162	c		—	0.0274	4.124	0.08	—	RV	2025
Barnard's Star^#	5.9629	9.51	0.162	e		—	0.0381	6.739	0.04	—	RV	2025
Lalande 21185^#	8.304		0.46	b		—	0.0788	12.94	0.06	—	RV	2019	1 candidate
Lalande 21185^#	8.304		0.46	c		—	2.94		0.13	—	RV	2021	1 candidate
Epsilon Eridani	10.501		0.82		318	—	3.53	2,680	0.06	40	RV	2000	1 inferred planet, 1 or possibly 2 inner debris discs, and an outer disc
Lacaille 9352^#	10.724		0.489	b		—	0.068	9.262	0.03	—	RV	2019	1 candidate
Lacaille 9352^#	10.724		0.489	c		—	0.120	21.79	0.03	—	RV	2019	1 candidate
Ross 128	11.007		0.168	b^↑		—	0.0496	9.866	0.12	—	RV	2017
Gliese 725 A	11.491	8.94	0.330	b	≥2.78	—	0.068	11.2201	0.0	—	RV	2024
Gliese 725 B	11.491	9.70	0.25	c	≥3.4	—	0.139	37.90	—	—	RV	2025
Groombridge 34 A^#	11.619		0.38	b		—	0.072	11.44	0.09	~54?	RV	2014
Groombridge 34 A^#	11.619		0.38	c		—	5.4		0.27	~54?	RV	2018
Epsilon Indi A	11.867		0.762	b	2005	—	28.4		0.40	103.7	RV	2018	nearest exoplanet directly imaged
GJ 1061^#	11.984		0.113	b		—	0.021	3.204	<0.31	—	RV	2019	two solutions for d's orbit
GJ 1061^#	11.984		0.113	c^↑		—	0.035	6.689	<0.29	—	RV	2019	two solutions for d's orbit
GJ 1061^#	11.984		0.113	d^↑		—	0.054	13.03	<0.53	—	RV	2019	two solutions for d's orbit
YZ Ceti^#	12.122		0.130	b		—	0.0163	2.021	0.06	—	RV	2017
YZ Ceti^#	12.122		0.130	c		—	0.0216	3.060	0.0	—	RV	2017
YZ Ceti^#	12.122		0.130	d		—	0.0285	4.656	0.07	—	RV	2017
Luyten's Star^#	12.348		0.29	c		—	0.0365	4.723	0.10	—	RV	2017	2 candidates
Luyten's Star^#	12.348		0.29	b^↑		—	0.0911	18.65	0.17	—	RV	2017	2 candidates
Teegarden's Star^#	12.497		0.08	b^↑		—	0.0259	4.906	0.03	—	RV	2019
Teegarden's Star^#	12.497		0.08	c^↑		—	0.0455	11.42	0.04	—	RV	2019
Teegarden's Star^#	12.497		0.08	d		—	0.0791	26.13	0.07	—	RV	2024
Wolf 1061^#	14.050		0.25	b		—	0.0375	4.887	0.15	—	RV	2015
Wolf 1061^#	14.050		0.25	c^↑		—	0.0890	17.87	0.11	—	RV	2015
Wolf 1061^#	14.050		0.25	d		—	0.470	217	0.55	—	RV	2015
TZ Arietis	14.578		0.14	b		—	0.88	771	0.46	—	RV	2019	2 refuted candidates
Gliese 687^#	14.839		0.41	b		—	0.163	38.14	0.17	—	RV	2014
Gliese 687^#	14.839		0.41	c		—	1.165	728	0.40	—	RV	2019
Gliese 674	14.849		0.35	b		—	0.039	4.694	0.20	—	RV	2007
Gliese 876^#	15.238		0.33	d	6.68	—	0.0210	1.938	0.04	56.7	RV	2005
Gliese 876^#	15.238		0.33	c	235	—	0.1309	30.10	0.26	56.7	RV	2000
Gliese 876^#	15.238		0.33	b	749	—	0.2098	61.10	0.03	56.7	RV	1998
Gliese 876^#	15.238		0.33	e	16	—	0.3355	123.6	0.05	56.7	RV	2010
GJ 1002^#	15.806		0.12	b^↑		—	0.0457	10.35	—	—	RV	2022
GJ 1002^#	15.806		0.12	c^↑		—	0.0738	21.2	—	—	RV	2022
Gliese 832	16.200		0.45	b	315	—	3.7		0.05	51 or 134	RV	2008	1 refuted candidate
GJ 3323^#	17.531		0.164	b		—	0.0328			—	RV	2017
GJ 3323^#	17.531		0.164	c		—	0.126			—	RV	2017
Gliese 251^#	18.215		0.372	b		—	0.0808		—	—	RV	2020
Gliese 251^#	18.215		0.372	c		—	0.196		—	—	RV	2025
Gliese 752 A	19.292		0.46	b		—	0.343		0.10	—	RV	2018
82 G. Eridani^#	19.704		0.79	b		—	0.126		0.06	—	RV	2011
82 G. Eridani^#	19.704		0.79	c		—	0.363		0.08	—	RV	2011
82 G. Eridani^#	19.704		0.79	d^↑		—	1.354		0.45	—	RV	2023
HN Librae	20.395		0.29	b		—	0.142		0.08	—	RV	2023	1 candidate
EQ Pegasi A	20.400		0.436	b		—	0.643		0.35	69.2	Astrometry	2022
Gliese 581^#	20.549		0.295	e		—	0.0280		0.01	47	RV	2009	3 refuted candidates and a disc
Gliese 581^#	20.549		0.295	b		—	0.0399		0.03	47	RV	2005	3 refuted candidates and a disc
Gliese 581^#	20.549		0.295	c		—	0.0718		0.03	47	RV	2007	3 refuted candidates and a disc
Gliese 338 B	20.658		0.64	b		—	0.141		0.11	—	RV	2020
Gliese 625	21.131		0.30	b		—	0.0784			—	RV	2017
HD 219134^#	21.336		0.78	b		1.60	0.0388			85.05	RV	2015	Has 1 candidate planet
HD 219134^#	21.336		0.78			1.51	0.065			87.28	RV	2015	Has 1 candidate planet
HD 219134^#	21.336		0.78			—	0.146			~87?	RV	2015	Has 1 candidate planet
HD 219134^#	21.336		0.78			—	0.237			~87?	RV	2015	Has 1 candidate planet
HD 219134^#	21.336		0.78			—	3.11			~87?	RV	2015	Has 1 candidate planet
LTT 1445 A^#	22.387		0.26	c		1.15	0.0266		<0.22	87.43	Transit	2021	1 candidate
LTT 1445 A^#	22.387		0.26	b		1.30	0.0381		<0.11	89.68	Transit	2019	1 candidate
Gliese 393	22.953		0.41	b		—	0.0540		0.00	—	RV	2019
Gliese 667 C^#	23.623		0.33			—	0.049		0.13	~52?	RV	2009	5 dubious candidates
Gliese 667 C^#	23.623		0.33	^↑		—	0.1251		0.03	~52?	RV	2011	5 dubious candidates
Gliese 514	24.878		0.53	b		—	0.421	140	0.45	—	RV	2022
GJ 1151	26.231		0.164	c		—	0.571	390	—	—	RV	2023	1 refuted candidate
Gliese 486	26.351		0.32			1.31	0.0173			88.4	Transit	2021
Gliese 686	26.613		0.42	b		—	0.097		0.04	—	RV	2019
GJ 1289	27.275	12.67	0.21	b		—	0.27	112	0	—	RV	2024
61 Virginis^#	27.836		0.95	b		—	0.05		0.05	~77?	RV	2009	a debris disc
61 Virginis^#	27.836		0.95	c		—	0.22		0.06	~77?	RV	2009	a debris disc
61 Virginis^#	27.836		0.95	d		—	0.47		0.12	~77?	RV	2009	a debris disc
CD Ceti	28.052		0.161	b		—	0.0185		0	—	RV	2020
Gliese 785^#	28.739		0.78	b		—	0.32		0.13	—	RV	2010
Gliese 785^#	28.739		0.78	c		—	1.18			—	RV	2011
Gliese 849^#	28.750		0.49	b		—	2.26		0.05	—	RV	2006
Gliese 849^#	28.750		0.49	c		—	4.82		0.087	—	RV	2006
Gliese 433^#	29.605		0.48	b		—	0.062		0.04	—	RV	2009
Gliese 433^#	29.605		0.48	d		—	0.178		0.07	—	RV	2020
Gliese 433^#	29.605		0.48	c		—	4.82		0.12	—	RV	2012
Gliese 367^#	30.719		0.45			0.70	0.0071		0.06	79.89	Transit	2021
Gliese 367^#	30.719		0.45	c		—	0.077	11.5	0.09	~80?	RV	2023
Gliese 367^#	30.719		0.45	d		—	0.159	34.4	0.14	~80?	RV	2023
Gliese 357^#	30.776		0.34	b		1.17	0.035	3.93	0.02	88.92	Transit	2019
Gliese 357^#	30.776		0.34	c		—	0.061	9.13	0.04	~89?	RV	2019
Gliese 357^#	30.776		0.34	d^↑		—	0.204	55.7	0.03	~89?	RV	2019
Gliese 176	30.937		0.45	b		—	0.066		0.08	—	RV	2007	1 disputed candidate
GJ 3512^#	30.976		0.123	b		—	0.338	204	0.44	—	RV	2019
GJ 3512^#	30.976		0.123	c		—	1.722		—	—	RV	2020
G 192-15^#	31.075		0.132	b		—	0.0172	2.275	0	—	RV	2025
G 192-15^#	31.075		0.132	c		—	1.137		0.68	—	RV	2025
Wolf 1069	31.229		0.167	b^↑		—	0.0672	15.56	—	—	RV	2023
AU Microscopii^#	31.683		0.50	b		4.38	0.0645		0.10	89.03	Transit	2020	2 candidates
AU Microscopii^#	31.683		0.50	c		3.51	0.1101		0	88.62	Transit	2020	2 candidates
Gliese 436	31.882		0.41			4.33	0.0280	2.64	0.15	85.8	RV	2004	One dubious candidate
G 268-110	31.888		0.137	b		—	0.0128	1.433	0	—	RV	2025
Gliese 49	32.158		0.57	b		—	0.106	17.3	0.03	—	RV	2019
GJ 3988	32.316		0.184	b		—	0.0405	6.944	0	—	RV	2023
HD 260655^#	32.608		0.439	b		1.240	0.0293		0.039	87.35	Transit	2022
HD 260655^#	32.608		0.439	c		1.533	0.0475		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,
Tau Ceti,
Gliese 682,
and HD 102365 A.
There are also several instances where proposed exoplanets were later disproved by subsequent studies, including candidates around Alpha Centauri B,
Kapteyn's Star,
Van Maanen 2,
Groombridge 1618,
AD Leonis,
40 Eridani A,
Gliese 229 A,
VB 10, and Fomalhaut.
A candidate planet around LHS 288 was proposed in 2007, but it has not been confirmed. 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. Candidate planets around, GJ 3378 and Achird were reported in 2024, 2024 and 2025, respectively.
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, SDSS J1416+1348 B, and WISE 1217+1626 B.
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, UGPS 0722-05, WISE 1541−2250, and SIMP J01365663+0933473.