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Lista de estrellas

        Nuestra galaxia, la Vía Láctea, contiene miles de millones de estrellas, desde estrellas masivas y brillantes hasta pequeños y tenues remanentes estelares. Algunas estrellas existen de forma independiente, mientras que muchas forman parte de sistemas binarios o múltiples. Esta página presenta una lista de las estrellas más cercanas al Sistema Solar, lo que ayuda a mapear nuestro vecindario estelar local y a comprender la diversidad de estrellas más cercanas a nosotros.

La lista se puede filtrar por categoría estelar, lo que permite explorar tipos específicos de estrellas, como enanas rojas, estrellas similares al Sol, enanas blancas o enanas marrones. Esta vista flexible facilita la comparación de diferentes poblaciones estelares y permite centrarse en objetos de interés. Si bien el enfoque principal se centra en las estrellas cercanas, el catálogo también se extiende más allá del vecindario inmediato, ofreciendo una perspectiva más amplia sobre los tipos de estrellas dentro de nuestra galaxia.
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Estrellas 541-560
>
Nombre de la estrella Mass Distance

Gliese 3668
LHS 306, LP 732-35, GJ 3668, 2MASS J11310835-1457201, NLTT 27616, WISEA J113108.68-145735.8
 M5 - 37.5 ly

UCAC4 427-122653
2MASS J21471744-0444406, TIC 24352777, WISEA J214717.63-044440.6, PM J21472-0444
 M4.0V - 37.5 ly

Gliese 3189
LHS 1481, GJ 3189, L 802-6, LP 711-32, LTT 1415, 2MASS J02581021-1253066, NLTT 9474, WISEA J025810.42-125300.3
 sdM3.0 0.24 M☉ 37.6 ly

2MASS J1246-3139
TIC 131308768, WISE J124629.65-313934.2, EQ J1246-3139, 2MASS J12462965-3139280
 T1 - 37.6 ly

ADS 48
HD 38, HIP 473, GJ 4, Gliese 4, CCDM J00057+4548AB, WDS J00057+4549AB, ADS 48 A, HD 38A, SAO 36046, GC 71, GJ 4 A, CCDM J00057+4548A, WDS J00057+4549A
 K6V C 0.5 M☉ 37.6 ly

Ross 119
GJ 9375, Gliese 9375, LFT 859, G 12-4, G 57-28, LHS 2472, LTT 13283, NLTT 28894, 2MASS J11540788+0948227, TIC 291108016, TYC 864-271-1, WISEA J115407.94+094814.2
 M4.0V - 37.6 ly

2MASS J2359-7335
TIC 293572002, WISEA J235941.10-733505.0, WISE J235941.07-733504.8, EQ J2359-7335, 2MASS J23594034-7335055
 T5.5 - 37.6 ly

MCC 568
HIC 49969, HIP 49969, G 53-28, G 162-24, G 55-2, GJ 381 B, LFT 698, LHS 2230, L 968-22, LP 609-71, LTT 3730, NLTT 23666, 2MASS J10120466-0241044, TIC 77610900, TYC 4907-91-1, WDS J10121-0241AB, WISEA J101205.04-024111.4
 M2.5V B - 37.6 ly

Ross 85
LHS 2173, AC +13 1301, G 42-17, GJ 361, Gliese 361, HIC 47513, HIP 47513, LFT 670, LTT 12562, NLTT 22345, 2MASS J09411033+1312344, TIC 307646256, TYC 827-1159-1, WISEA J094109.88+131232.9
 M2.5V - 37.7 ly

V* CC Eri
HD 16157, CABS 19, CD-44 775, 2E 592, GC 3097, GJ 103, Gliese 103, HIC 11964, HIP 11964, IRAS 02324-4400, LTT 1261, 2MASS J02342256-4347467, NLTT 8399, RBS 328, TIC 142206123, TYC 7558-585-1, UGP 39, WEB 2471, WISEA J023422.64-434749.8
 K7V - 37.7 ly

Gliese 842
LHS 3741, DENIS J215934.4-594509, GJ 842, CD-60 7821, HIC 108569, HIP 108569, LFT 1672, L 165-2, LTT 8780, NLTT 52576, 2MASS J21593479-5945104, TIC 394015919, TYC 8820-224-1, WISEA J215935.92-594511.3
 M0.5V 0.58 M☉ 37.7 ly

SSSPM J1358-3938
2MASS J13580529-3937545, TIC 178930081, WISEA J135806.95-393804.2
 M3.5 d - 37.7 ly

WISE J0623-0456
WISE J062309.94-045624.6, ASKAP J062309.2−0456227
 T8 0.01 M☉ 37.7 ly

LAWD 79
GJ 772, Gliese 772, G 92-40, LFT 1503, LHS 3501, L 997-21, LP 634-1, LTT 7879, NLTT 48454, 2MASS J19562925-0102317, SDSS J195629.08-010236.0, TIC 251903434, WD 1953-011
 DA6.4 - 37.7 ly

HD 75632
BD+71 482A, G 252-24A, GC 12268, GJ 325, Gliese 325, HIC 43820, HIP 43820, 2MASS J08552479+7047389, WISE J085522.07+704735.1
 M1V - 37.8 ly

2MASS J02511490-0352459
2MASS J02511490-0352459, 2MUCD 10151, SDSS J025115.51-035300.9, TIC 10934710, WISE J025115.76-035307.0
 L3 - 37.8 ly

2MASS J2224-0158
2MASS J22244381-0158521, 2MASSW J2224438-015852, TIC 176006315
 L4.5V - 37.9 ly

SCR J1855-6914
2MASS J18554792-6914153, DENIS J185548.0-691415, TIC 381983159, WISEA J185548.76-691422.2
 M6e D - 37.9 ly

Wolf 230
G 97-20, G 85-41, GJ 3333, Gliese 3333, LTT 11586, NLTT 14527, 2MASS J05074924+1758584, TIC 27137427, WISEA J050749.30+175855.0
M2V - 37.9 ly

DE Bootis
HD 131511, GC 20037, GJ 567, Gliese 567, HIC 72848, HIP 72848, HR 5553, LAL 27137, LFT 1153, LHS 5279, LTT 14413, 2MASS J14532374+1909104, NLTT 38694, SAO 101276, TIC 267365256, TYC 1481-694-1, WISEA J145323.43+190912.4, V* DE Boo
 K0.5V - 37.9 ly
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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: Estrellas

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Estrellas
Las estrellas son enormes esferas de gas caliente que brillan al generar energía mediante fusión nuclear en sus núcleos. La mayoría de las estrellas están compuestas principalmente de hidrógeno y helio. En el centro de una estrella, la alta presión y temperatura hacen que los átomos de hidrógeno se fusionen en helio, liberando una enorme cantidad de energía en forma de luz y calor.
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Random terms
Posición de la estrellaLuminosidadTemperatura de la estrellaMasa estelarTamaño de la estrellaEdad de las estrellas

Evolución estelar

Stars are born and die in various ways depending on their mass, composition, and other factors. The most common life cycle for stars like our Sun involves several key stages.
Stellar evolution visualisation

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