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List of nearest Sun-like stars

          This page focuses on Sun-like stars near the Solar System, which are especially important in astronomy because they resemble the environment in which life developed on Earth. G-type stars are stable over billions of years and can host planetary systems with a wide range of planets. Studying nearby Sun-like stars helps scientists compare other systems to our own and assess where conditions similar to those around the Sun may exist elsewhere in the galaxy.
    
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Stars 41-60
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Star name Mass Distance

Nu2 Lupi
ν2 Lup, CD−47° 9919, Gaia DR2 5902750168276592256, GJ 582, HD 136352, HIP 75181, HR 5699, SAO 225697
G3/5V 0.86 M☉ 48.1 ly

Psi Serpentis
ψ Ser, 23 Ser, BD+02° 2989, FK5 3248, GJ 9527, Gliese 9527, HD 140538, HIP 77052, HR 5853, SAO 121152
G2.5V 0.99 M☉ 48.2 ly

20 Leonis Minoris
20 LMi, BD+32° 1964, FK5 1258, GJ 376, Gliese 376, HD 86728, HIC 49081, HIP 49081, HR 3951, SAO 61808, LHS 2216, LTT 12671
G3VaHdel1 0.97 M☉ 48.7 ly

HD 4391
CD-48 176, HD 4391, Gliese 1021, GJ 1021, HIP 3583, HR 209, SAO 215232
G3V 1.2 M☉ 49.1 ly

HD 122742
TYC 904-1278-1, HIC 68682, HIP 68682, Gliese 538, GJ 538, 2MASS J14033235+1047121, HR 5273, PLX 3201, UBV 12441, AG +11 1547, PPM 130282, UBV M 19939, ASCC 956692, SAO 100832, USNO -B1.0 1007-00222108, BD +11 2625, IRAS 14010+1101, SBC9 799, uvby98 100122742, GC 18985, LSPM J1403+1047, YZ 11 5003, GCRV 8257, LTT 14110, SPOCS 588, TD1 17224
G6V 0.96 M☉ 49.3 ly

HD 38858
NS 0548-0405, Gliese 1085, GJ 1085, HIP 27435, HD 38858, HR 2007, BD-04 1244, LTT 2380, 1RXS J054837.7-040550
G2V 0.89 M☉ 49.6 ly

HD 3443
CD-25 225, CPD CPD-25 64, GJ 25, Gliese 25, HIP 2941, HR 159, 2MASS J00372057-2446023, WDS 00373–2446, Gaia EDR3 2347260998051944448, TYC 6421-1924-1
G9V 0.92 M☉ 50.2 ly

HD 207129
CCDM J21483-4718A, CD−47 13928, CPD−47 9758, FK5 1573, GC 30516, Gliese 838, GJ 838, HR 8323, HIP 107649, IDS 21418-4746 A, LTT 8704, NLTT 52100, PPM 327579, SAO 230846, WDS J21483-4718A
G2V 0.97 M☉ 50.7 ly

Gliese 758
GJ 758, BD+32 3411, HD 182488, HIP 95319, HR 7368, PPM 82821, SAO 68239
G8V 0.97 M☉ 50.9 ly

m Tauri
GJ 188, Gliese 188, HD 32923, HIP 23835, LFT 388, LHS 1736, LTT 11583, 2MASS J05072692+1838420, TIC 27136704, TYC 1286-403-1, YZ 18 1399
G4V - 51.9 ly

Gliese 777
BD+29°3872, GJ 777, HD 190360, HIC 98767, HIP 98767, HR 7670, LHS 3510, GJ 9683, Gliese 9683, 2MASS J20033732+2953493, TIC 105999792, TYC 2153-2883-1, WISEA J200337.97+295343.4
G7IV-V C 0.82 M☉ 52.2 ly

10 Ursae Majoris B
K0V 0.89 M☉ 52.4 ly

9 Puppis
BU 101, 9 Pup, BD−13° 2267, GC 10629, Gliese 291, GJ 291, HD 64096, HIP 38382, HR 3064, SAO 153500, ADS 6420, WDS J07518-1354, 2MASS J07514629-1353526
G1V 1.1 M☉ 53.8 ly

9 Puppis B
G9V 0.9 M☉ 53.8 ly

HD 116442
HIP 65352, GJ 3781, Gliese 3781, TYC-303-1283-1, BD +03 2765
G9V - 54.1 ly

HD 43162
PPM 250051, CD -23 3577, HD 43162, TYC 6505-2273-1, CPD -23 1125, HIC 29568, HIP 29568, HR 2225, RE J061344-235223, uvby98 100043162, GC 7961, IRAS 06116-2350, SAO 171428, YZ 113 3371, 2MASS J06134528-2351433, Gliese 3389, GJ 3389, NSV 16808, SRS 6921
G6.5V 0.97 M☉ 54.5 ly

HD 152391
V2292 Ophiuchi, 2MASS J16525877-0001356, BD+00 3593, GJ 641, Gliese 641, HIP 82588, LFT 1307, LHS 426, TYC 5051-1354-1
G8.5Vk: - 54.8 ly

39 Tauri
39 Tau, BD+21 587, GJ 160, Gliese 160, HD 25680, HIP 19076, HR 1262, SAO 76438, A2 Tauri
G5V 1.1 M☉ 54.8 ly

HD 76151
BD−04 2490, GC 12307, GJ 327, Gliese 327, HIP 43726, HR 3538, LTT 3283, NLTT 20504, PPM 191823, SAO 136389
G2V 0.92 M☉ 54.9 ly

HD 177565
LTT 7569, NLTT 47394, CD-37 13049, GJ 744, Gliese 744, HIC 93858, HIP 93858, HR 7232, 2MASS J19065247-3748380, SAO 210937, TIC 254147274, TYC 7917-565-1
G6V 1 M☉ 55.3 ly
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Sun-like stars news

Stellar obliquity in Sun-like stars remains stable throughout planetary system development
iconYesterday
iconStars | Exoplanets | Sun-like star
Image: Stellar obliquity in Sun-like stars remains stable throughout planetary system development
Stellar obliquity refers to the angle between the direction of a star's rotation and the orbital plane of its planets. This measurement acts like a historical record, revealing the initial conditions and the dynamical evolution of a planetary system. When this angle is high, it indicates that the star and its planets are misaligned, which can happen if a star's early environment was turbulent or if outside forces later disturbed the planets' paths. To understand how these angles change over t...
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Earth-like planet masses remain hard to measure around Sun-like stars
icon29. 10. 2026
iconStars | Exoplanets | Sun-like stars | PLATO
Image: Earth-like planet masses remain hard to measure around Sun-like stars
The PLATO radial-velocity data challenge found that measuring habitable-zone planet masses around Sun-like stars to better than 10% is typically difficult below 8 to 10 Earth masses. Around orange dwarfs, the comparable range may reach 2 to 5 Earth masses....
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Deep learning estimates a non-transiting companion in the Kepler-88 system
icon28. 10. 2026
iconStars | Exoplanets | Sun-like stars | Kepler
Image: Deep learning estimates a non-transiting companion in the Kepler-88 system
Kepler-88-based tests show a deep-learning method can estimate a non-transiting planet’s orbit and mass from transit timing and duration changes. Errors varied by property, reaching about 10% or less for orbital size and eccentricity and roughly 10–30% for mass....
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study iconResearch in Sun-like stars

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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: Stars

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Stars
Stars are enormous spheres of hot gas that shine by generating energy through nuclear fusion in their cores. Most stars are made primarily of hydrogen and helium. In the center of a star, intense pressure and temperature cause hydrogen atoms to fuse into helium, releasing a tremendous amount of energy as light and heat.
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Stellar categories

A comparison of spectral classes and typical stellar properties across the catalog categories.
Category Spectral class Typical mass (% of solar mass) Typical size (% of solar radius) Typical temperature (K)
, , 10-200% 50-300% 2000-10000 K
L, T, Y 1.2-8.0% 9-11% 600-2500 K
M 7.5-50% 10-60% 2400-3900 K
K 50-80% 60-90% 3900-5200 K
G 80-120% 80-120% 5200-6000 K
A, F, B, O 200-3000% 200-5000% 7000-40000 K
K|G|F|A|B 80-150% 120-300% 4500-6000 K
A|B|O, G|F|A, M|G|F|A, K|M|S 50-300% 500-20000% 3000-5000 K
K|M|C, G|F, B|O 500-10000% 10000-100000% 3000-35000 K
A|B, G|F, K|M 2000-20000% 50000-200000% 3000-40000 K
WC|WN|WO 1000-10000% 50-500% 30000-200000 K
DA|DC|DQ|DZ 20-140% 0.7-1.5% 5000-150000 K
100-300% 0.001-0.002% 600000-1000000 K
, , 300-10000000% 0.000001-1% 0-10000000 K

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