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Etoile 381-400
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Nom de l étoile Mass Distance

Wolf 1561 B
LHS 3788, LDS 782B, EPIC 206262223, LFT 1700, L 932-39, LP 759-82, LTT 8939, 2MASS J22171870-0848186, NLTT 53398, WISEA J221718.35-084821.4
 M5V - 36.3 ly

BD+47 2112
LHS 2849, ADS 9090 A, G 200-16A, GJ 537 A, Gliese 537, LFT 1065, LTT 14107, 2MASS J14023312+4620239, NLTT 36091, TIC 198151134, TYC 3465-617-1
 M2V - 36.4 ly

BD+47 2112 B
LHS 2850, LFT 1066, LTT 14108, NLTT 36092, 2MASS J14023324+4620266, TIC 198151136, TYC 3465-617-2, WDS J14024+4620B
 M2.5V - 36.4 ly

Theta Persei B
2MASS J02441025+4913540
 M1.5V 0.52 M☉ 36.5 ly

L 380-8
LHS 1831, GJ 1088, Gliese 1088, LFT 460, LTT 2480, NLTT 16205, 2MASS J06105288-4324178, TIC 231917352, WISEA J061053.00-432410.0
 M4e - 36.5 ly

L 762-51
LHS 2794, EPIC 212285603, GJ 3804, Gliese 3804, HIC 67164, HIP 67164, LFT 1035, L 762-51, LP 798-34, LTT 5346, 2MASS J13455074-1758047, NLTT 35132, TIC 286942673, TYC 6127-534-1
 dM3.5 - 36.5 ly

L 136-37
LTT 2816, NLTT 17788, 2MASS J07205204-6210118, DENIS J072051.9-621011, TIC 349374765, WISEA J072051.59-621009.5
 M3 - 36.6 ly

Gliese 173
GJ 173, BD-11 916, LP 715-52, GCRV 2717, HIC 21556, HIP 21556, LTT 2050, 2MASS J04374188-1102198, MCC 106, NLTT 13657, TIC 55997717, TYC 5324-581-1, WEB 4138
 M1V 0.48 M☉ 36.6 ly

Ross 508
LHS 396, G 137-2, G 136-103, GJ 585, Gliese 585, JP11 5158, LFT 1203, LTT 14584, 2MASS J15235112+1727569, NLTT 40124, TIC 400019820, WISEA J152350.85+172744.4
 M4.92 0.18 M☉ 36.6 ly

UCAC4 608-044702
2MASS J08401597+3127068, TIC 341526939, LSPM J0840+3127
 M3.5Ve - 36.6 ly

HD 28343
GJ 169, Gliese 169, HIC 20917, HIP 20917, LTT 11433, NLTT 13343, 2MASS J04290013+2155214, TIC 17558287, TYC 1277-601-1, WISEA J042900.05+215523.6
 M0.5V - 36.6 ly

11 Leonis Minoris B
 M4 0.23 M☉ 36.7 ly

Gliese 3959
2E 3717, G 180-60, HAT 193-01110, NLTT 43010, 2MASS J16311879+4051516, SDSS J163118.77+405152.1, NN 3959, GJ 3959
 M6 V 0 M☉ 36.7 ly

G 107-69
LHS 229, G 111-7, G 193-50, GJ 275.2 A, Gliese 275.2 A, 2MASS J07304280+4811599, NLTT 17949, TIC 328328639, WISEA J073042.55+481145.2
 M4V - 36.8 ly

LP 625-34
GJ 3967, Gliese 3967, 2MASS J16400599+0042188, NLTT 43307, TIC 281935723,
M5V - 36.8 ly

PM J17189-4131
DENIS J171854.5-413140, 2MASS J17185456-4131395, TIC 192642951, WISEA J171854.33-413149.6
 M6 - 36.8 ly

PM J19515-3510 B
 - 36.9 ly

G 3-14
LHS 1290, G 71-28, GJ 70, Gliese 70, HIC 8051, HIP 8051, LFT 1851, LTT 10604, NLTT 5733, 2MASS J01432015+0419172, TIC 369534824, TYC 32-1005-1, WISEA J014319.89+041910.0
 M2V - 36.9 ly

LP 938-71
DENIS J010250.6-373744, LHS 132, 2MASS J01025100-3737438, NLTT 3459, TIC 180724005, WISEA J010252.38-373741.0
 M8.0V - 36.9 ly

PM J19515-3510
NSN 488A, WDS J19516-3511A
 M4 D - 37 ly
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Naines rouges nouvelles

Sub-Earth-sized planet candidate observed around the red dwarf Gliese 774
iconYesterday
iconÉtoiles | Exoplanètes | Naines rouges | TESS
Image: Sub-Earth-sized planet candidate observed around the red dwarf Gliese 774
A small planet candidate has been identified in the binary star system known as Gliese 774. The object, which is smaller than the Earth, orbits its host star approximately every 4.2 days. Observations from the Transiting Exoplanet Survey Satellite (TESS) captured the planet as it passed in front of its star, briefly blocking a tiny fraction of the starlight. This periodic dimming event allowed for the identification of the candidate despite the complex environment of a binary system, where two s...
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Ammonia and hydrogen may separate inside Uranus and Neptune
iconYesterday
iconÉtoiles | Exoplanètes | Naines rouge
Image: Ammonia and hydrogen may separate inside Uranus and Neptune
Uranus and Neptune may be experiencing ammonia rain: simulations show their expected temperature profiles cross the boundary where ammonia and hydrogen separate. In warmer sub-Neptune TOI-270 d, the two are likely to mix in all proportions....
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Orbital and atmospheric evolution of the mini-Neptune TOI-2257 b
icon15. 10. 2026
iconÉtoiles | Exoplanètes | Naines rouges | Super-Terre | Atmosphères planétaires | TESS
Image: Orbital and atmospheric evolution of the mini-Neptune TOI-2257 b
The exoplanet TOI-2257 b orbits its star once every 35 days with a high eccentricity. New models suggest its atmospheric and orbital fate depends on whether it is a gas-rich mini-Neptune or a rocky super-Earth. Higher eccentricity would confirm a gaseous nature....
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study iconResearch in Naines rouges

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Parcourez les dernières études scientifiques sur les étoiles et les exoplanètes de notre galaxie. Découvrez les dernières recherches en astrophysique et en astronomie stellaire.
Les recherches en cours

 TIC 220432308
1129 ly
 +1 study icon Two Validated Planets and 179 Candidates From a TESS Faint Star Transit Search in the ULTRASAT Fields
yesterday

TOI 431
106 ly
 +4 study icon Thermal Evolution of Lava Planets Across System Ages: Predictions for Hell of a Survey
yesterday

L 115-21
41.9 ly
 study icon A sub-Earth-sized TESS planet candidate in the nearby M-dwarf binary GJ 774, most likely orbiting GJ 774 A (TIC 351339274)
yesterday

TOI-3686
841 ly
 study icon TOI-3686: A Hot Jupiter and Sub-Neptune In A 2:1 Mean-Motion Resonance
yesterday

HD 112485
5881 ly
 study icon Ensemble pulsational characteristics of eclipsing binaries containing β Cep stars observed by the TESS mission
19. 10. 2026
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Publications plus anciennes

Frequently Asked Questions about nearby stars

What is the nearest star?

Nearest star is Proxima Centauri, located approximately 4.24 light-years (1.30 parsecs) from the Sun. It is part of the Alpha Centauri star system, which also includes Alpha Centauri A and Alpha Centauri B.

What are the nearest stars to Earth?

Nearest stars to Earth include the Alpha Centauri system (Alpha Centauri A, Alpha Centauri B, and Proxima Centauri), Barnard's Star, and Wolf 359. There are also brown dwarfs Luhman 16 and WISE 0855−0714.

What is the solar neighborhood?

Solar neighborhood (also Local Interstellar Cloud) is the region of interstellar space that surrounds the Sun with diameter about 15 light years. Stellar Catalog database includes all stars contained within this region.

How do astronomers measure distances to stars?

Astronomers use methods like parallax, standard candles, and redshift to measure distances to stars. Parallax is especially useful for nearby stars in our solar neighborhood, while other techniques help map the universe beyond.

Are there any exoplanets orbiting the nearest stars?

Yes, several exoplanets have been discovered orbiting the nearest stars. For example, Proxima Centauri has an exoplanet called Proxima Centauri b, which is located in the star's habitable zone and is the closest known exoplanet to Earth.

Why are the nearest stars important for astronomy and physics?

The nearest stars provide valuable laboratories for studying stellar evolution, space environments, and the fundamental physics of stars. Observing these stars helps astronomers understand the structure of our galaxy and the broader universe.
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exoplanet iconStellarGuide: Étoiles

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Étoiles
Les étoiles sont d’immenses sphères de gaz chaud qui brillent en produisant de l’énergie grâce à la fusion nucléaire dans leur noyau. La plupart des étoiles sont composées principalement d’hydrogène et d’hélium. Au centre d’une étoile, la pression et la température élevées provoquent la fusion des atomes d’hydrogène en hélium, libérant ainsi une énorme quantité d’énergie sous forme de lumière et de chaleur.
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Random terms
Position de la étoileLuminositéTempérature des étoilesMasse stellaireTaille de l´étoileL´âge des étoiles

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