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Seznam nejbližších Červení trpaslíci

        
    
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Hvězdy 241-260
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Název hvězdy Mass Distance

2MASS J2049-4012
2MASS J20490993-4012062, UCAC3 100-409084, SCR J2049-4012, BPS CS 22879-0089, TIC 389426731
0 M☉ 31 ly

Gliese 1123
LHS 263, LFT 640, L 35-12, LTT 3435, 2MASS J09170532-7749233, NLTT 21495
M4.5 V 0.1 M☉ 31.1 ly

Gliese 3380
LHS 1809, G 192-15, NLTT 15934, 2MASS J06022918+4951561
M6V 0.14 M☉ 31.1 ly

Gliese 1256
YPC 4929.11, LHS 495, G 144-25, NLTT 49676, WISEA J204034.83+153005.8
M4.5 V 0.19 M☉ 31.1 ly

Gliese 694
LHS 3321, BD+43 2796, G 204-27, HIC 86776, HIP 86776, LFT 1371, LTT 15258, MCC 171, NLTT 45376, 2MASS J17435595+4322441
M2 V 0 M☉ 31.1 ly

G 42-24
GJ 3571, G 54-2, G 42-24, G 49-26, LHS 2206, NLTT 22870, 2MASS J09535523+2056460, PM 09512+2111, TIC 88099283, WISEA J095354.91+205650.9, Gaia DR2 628080246633611520
M4.0Ve - 31.1 ly

Gliese 1253
LHS 3549, NLTT 49289, Wolf 1069, GJ 1253
dM5.0 C 0.17 M☉ 31.2 ly

PM J20502-3424
UCAC4 278-227158, 2MASS J20501615-3424424, TIC 89257479, Gaia DR2 677982100305845312
M5e - 31.3 ly

Gliese 358
CD-40 5404, TDS 6725, CF 20558, CPD-40 3789, HIC 47425, HIP 47425, JP11 329, LFT 666, LHS 2166, L 390-5, LPM 323, LTT 3547, NLTT 22318, 2MASS J09394631-4104029
M3 V 0 M☉ 31.3 ly

Gliese 3253
Wolf 227, G 6-39, LFT 317, LHS 1610, LTT 11284, NLTT 12056, 2MASS J03524169+1701056
M5 V 0.17 M☉ 31.5 ly

Gliese 680
CD-48 11837, LTT 6988, SKF 104, CF 16879, HIC 86057, HIP 86057, NLTT 45045, NSV 9166
M3 V 0 M☉ 31.6 ly

Gliese 680 B
M3V - 31.6 ly

Gliese 595
HIP 76901, HIC 76901, JP11 5188, JP11 5159, L 768-119, LFT 1218, LHS 54, LTT 6273, NLTT 40918, 2MASS J15420677-1928167, GJ 595
M3 D 0.29 M☉ 31.6 ly

AU Microscopii
AU Mic, Gliese 803, GJ 803, LDS 720A, HD 197481, HIC 102409, HIP 102409, LTT 8214, NLTT 49807, MCC 824, 2MASS J20450949-3120266, TOI-2221, TIC 441420236
M1 Ve 0.5 M☉ 31.7 ly

2MASS J20304235+0749358
PSO J307.6784+07.8236, TIC 374469464, WISE J203042.79+074934.7, EQ J2030+0749
T1.5 - 31.7 ly

Gliese 1138
LHS 293, LFT 740, L 1545-74, LP 263-29, LTT 12885, NLTT 25434, G 146-67, 2MASS J10494561+3532515, GJ 1138, G 119-36
M5 V - 31.7 ly

LP 655-48
DENIS J044023.1-053009, 2MASS J04402325-0530082, 2MUCD 10316, NLTT 13728, TIC 298907057
M7.5Ve - 31.8 ly

Gliese 436
2MASS J11421096+2642251, GJ 436, HIP 57087, LTT 13213, LHS 310, Ross 905, G 120-68, LFT 838, NLTT 28288, WISEA J114211.79+264215.1
M3V 0.41 M☉ 31.9 ly

Gliese 1028
LHS 134, G 268-110, NLTT 3576, 2MASS J01045368-1807292, GJ 1028, Gliese 1028
M6V 0.14 M☉ 31.9 ly

V* AT Mic B
LTT 8182, GJ 799 B, NLTT 49691, Gaia DR2 6792436799477051904, LDS 720C, CD-32 16135B
M4.5Ve - 32 ly
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Červení trpaslíci zprávy

Sub-Earth-sized planet candidate observed around the red dwarf Gliese 774 A
iconToday
iconHvězdy | Exoplanety | Červení trpaslíci | TESS
Image: Sub-Earth-sized planet candidate observed around the red dwarf Gliese 774 A
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
iconToday
iconHvězdy | Exoplanety | Červení trpaslíci
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
iconHvězdy | Exoplanety | Červení trpaslíci | Superzemě | Atmosféry planet | 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 Červení trpaslíci

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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: Hvězdy

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Hvězdy
Hvězdy jsou obrovské koule horkého plynu, které září díky energii vznikající jadernou fúzí v jejich jádru. Většina hvězd se skládá převážně z vodíku a helia. V centru hvězdy dochází díky vysokému tlaku a teplotě k přeměně vodíku na helium, přičemž se uvolňuje obrovské množství energie ve formě světla a tepla.
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