Étoiles massives de la séquence principale

	Mass	Distance
HD 199260 GJ 811, Gliese 811	F6V	-	68.8 ly
50 Persei 50 Per, BD+37° 882, FK5 2297, Gliese 9145, GJ 9145, HD 25998, HIC 19335, HIP 19335, HR 1278, SAO 57006	F8V	1.2 M☉	69.1 ly
HD 200525 TYC 9333-1274-1, LHS 3635, HIP 104440, HR 8061, Gliese 818.1 B	F9.5V	-	69.4 ly
I Puppis GJ 9225, Gliese 9225, QW Puppis, 71 Puppis, TYC 8119-2547-1, HIP 34834, HR 2740, TIC 134497068	F3VFe-1.0	-	69.5 ly
Theta Sculptoris θ Scl, CD−35°4, FK5 6, GC 202, GJ 3013, HD 739, HIP 950, HR 35, SAO 192388, LTT 79, GSC 06995-01262	F5V	1.3 M☉	70.8 ly
HD 16673 HIP 12444, GJ 3175, Gliese 3175, PPM 184889, UBV M 9092, BD -10 525, GSC 05285-01109, ROT 363, uvby98 100016673, 2EUVE J0240-09.4, SAO 130047, YZ 0 4897, EUVE J0240-09.4, HIC 12444, YZ 99 595, GC 3216, HR 784, TD1 1574, GCRV 1506, IRAS 02377-0940, TYC 5285-1109-1, 2MASS J02401242-0927103, UBV 2649	F8VFe-0.4	1.1 M☉	71 ly
Kappa Reticuli κ Ret, 4 Ret, CD−63° 112, FK5 126, HD 22001, HIP 16245, HR 1083, SAO 248819, WDS J03294-6256A	F3IV/V	1.3 M☉	71 ly
Alpha Hydri α Hyi, CD−62° 71, GJ 83, Gliese 83, HIP 9236, HR 591, SAO 248474	F0IV	2 M☉	71.8 ly
Epsilon Serpentis ε Ser, 37 Serpentis, BD+04°3069, HD 141795, HIP 77622, HR 5892, SAO 121218	kA2hA5mA7V	1.8 M☉	72 ly
Y Velorum GJ 9332, Gliese 9332, HD 91324, HIP 51523, TIC 447823435, TYC 8601-4516-1, WISEA J103121.36-534253.4, HR 4134, SAO 238146	F9VFe-0.8CH-0.7	1.2 M☉	72 ly
Mu1 Cygni 78 Cyg, BD+28°4169, HIP 107310, CCDM J21442+2845AB, WDS J21441+2845AB, HD 206826, HR 8309, SAO 89940	F6V+F3V	1.3 M☉	72.2 ly
HD 189245 262 G. Sgr[8], CD−34° 14082, GJ 773.4, Gliese 773.4, 9679, HD 189245, HIP 98470, HR 7631, SAO 211724	F8.5 V Fe−0.6 CH	-	72.2 ly
39 Leonis 39 Leo, BD+23 2207, GJ 387, Gliese 387, HD 89125, HIP 50384, HR 4039, SAO 81270	F6V	0.98 M☉	72.6 ly
84 Ceti 84 Cet, BD–01 377, HD 16765, HIP 12530, HR 790, SAO 130055	F7V	1.2 M☉	72.7 ly
HD 108954 BD+53 1554，SAO 28413，HR 4767	F9V	-	72.8 ly
Zeta Leporis	A2IV-V(n)	1.5 M☉	72.8 ly
HD 106516 BD-09 3468，SAO 157168，HR 4657	F9VFe-1.7CH-0.7	-	72.9 ly
18 Puppis GJ 9255, Gliese 9255, HD 68146, HIP 40035, HR 3202, TIC 422142487, TYC 5438-2380-1,	F6.5V	-	73.6 ly
Gamma Tucanae γ Tuc, CPD−58° 8062, FK5 877, GC 32413, GJ 9818, Gliese 9818, HD 219571, HIP 114996, HR 8848, SAO 247814, GSC 08837-01297	F4V	1.6 M☉	74 ly
Sigma Coronae Borealis σ CrB, 17 CrB, BD+34° 2750, HIP 79607 (only AB), SAO 65165, ADS 9979, σ2 CrB, TZ CrB, GJ 9550B, Gliese 9550B, HD 146361, HR 6064, CCDM J16147+3352A, WDS J16147+3352A, TYC 2583-1846-1	F6V	1 M☉	74 ly

Nom de l étoile

Mass

Distance

HD 199260

GJ 811, Gliese 811

F6V

68.8 ly

50 Persei

50 Per, BD+37° 882, FK5 2297, Gliese 9145, GJ 9145, HD 25998, HIC 19335, HIP 19335, HR 1278, SAO 57006

F8V

1.2 M☉

69.1 ly

HD 200525

TYC 9333-1274-1, LHS 3635, HIP 104440, HR 8061, Gliese 818.1 B

F9.5V

69.4 ly

I Puppis

GJ 9225, Gliese 9225, QW Puppis, 71 Puppis, TYC 8119-2547-1, HIP 34834, HR 2740, TIC 134497068

F3VFe-1.0

69.5 ly

Theta Sculptoris

θ Scl, CD−35°4, FK5 6, GC 202, GJ 3013, HD 739, HIP 950, HR 35, SAO 192388, LTT 79, GSC 06995-01262

F5V

1.3 M☉

70.8 ly

HD 16673

HIP 12444, GJ 3175, Gliese 3175, PPM 184889, UBV M 9092, BD -10 525, GSC 05285-01109, ROT 363, uvby98 100016673, 2EUVE J0240-09.4, SAO 130047, YZ 0 4897, EUVE J0240-09.4, HIC 12444, YZ 99 595, GC 3216, HR 784, TD1 1574, GCRV 1506, IRAS 02377-0940, TYC 5285-1109-1, 2MASS J02401242-0927103, UBV 2649

F8VFe-0.4

1.1 M☉

71 ly

Kappa Reticuli

κ Ret, 4 Ret, CD−63° 112, FK5 126, HD 22001, HIP 16245, HR 1083, SAO 248819, WDS J03294-6256A

F3IV/V

1.3 M☉

71 ly

Alpha Hydri

α Hyi, CD−62° 71, GJ 83, Gliese 83, HIP 9236, HR 591, SAO 248474

F0IV

2 M☉

71.8 ly

Epsilon Serpentis

ε Ser, 37 Serpentis, BD+04°3069, HD 141795, HIP 77622, HR 5892, SAO 121218

kA2hA5mA7V

1.8 M☉

72 ly

Y Velorum

GJ 9332, Gliese 9332, HD 91324, HIP 51523, TIC 447823435, TYC 8601-4516-1, WISEA J103121.36-534253.4, HR 4134, SAO 238146

F9VFe-0.8CH-0.7

1.2 M☉

72 ly

Mu1 Cygni

78 Cyg, BD+28°4169, HIP 107310, CCDM J21442+2845AB, WDS J21441+2845AB, HD 206826, HR 8309, SAO 89940

F6V+F3V

1.3 M☉

72.2 ly

HD 189245

262 G. Sgr[8], CD−34° 14082, GJ 773.4, Gliese 773.4, 9679, HD 189245, HIP 98470, HR 7631, SAO 211724

F8.5 V Fe−0.6 CH

72.2 ly

39 Leonis

39 Leo, BD+23 2207, GJ 387, Gliese 387, HD 89125, HIP 50384, HR 4039, SAO 81270

F6V

0.98 M☉

72.6 ly

84 Ceti

84 Cet, BD–01 377, HD 16765, HIP 12530, HR 790, SAO 130055

F7V

1.2 M☉

72.7 ly

HD 108954

BD+53 1554，SAO 28413，HR 4767

F9V

72.8 ly

Zeta Leporis

A2IV-V(n)

1.5 M☉

72.8 ly

HD 106516

BD-09 3468，SAO 157168，HR 4657

F9VFe-1.7CH-0.7

72.9 ly

18 Puppis

GJ 9255, Gliese 9255, HD 68146, HIP 40035, HR 3202, TIC 422142487, TYC 5438-2380-1,

F6.5V

73.6 ly

Gamma Tucanae

γ Tuc, CPD−58° 8062, FK5 877, GC 32413, GJ 9818, Gliese 9818, HD 219571, HIP 114996, HR 8848, SAO 247814, GSC 08837-01297

F4V

1.6 M☉

74 ly

Sigma Coronae Borealis

σ CrB, 17 CrB, BD+34° 2750, HIP 79607 (only AB), SAO 65165, ADS 9979, σ2 CrB, TZ CrB, GJ 9550B, Gliese 9550B, HD 146361, HR 6064, CCDM J16147+3352A, WDS J16147+3352A, TYC 2583-1846-1

F6V

1 M☉

74 ly

Étoiles massives de la séquence principale nouvelles

Lambda Bootis phenomenon identified in the massive early B-type star HD 37356

10. 8. 2026

Étoiles | Étoiles massives de la séquence principale

Image: Lambda Bootis phenomenon identified in the massive early B-type star HD 37356

The Lambda Bootis phenomenon is a unique chemical condition in stars where certain elements, known as refractory elements (materials that condense at high temperatures, such as iron), are significantly less abundant than expected, while volatile elements remain at normal levels. This feature has now been identified in the massive early B-type star HD 37356, marking the first time this characteristic has been observed in such a massive stellar object. Researchers analyzed high-quality spectra ...

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Circumstellar disks observed around five massive Herbig Be stars

24. 6. 2026

Étoiles | Étoiles massives de la séquence principale | Formation des planète

Image: Circumstellar disks observed around five massive Herbig Be stars

A survey of 24 massive Herbig Be stars identifies circumstellar disks around 5 of them. These disks contain enough material to potentially form giant planets, following scaling laws similar to those seen in lower-mass young stars....

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HD 48914 binary system characteristics measured via photometric and radial velocity data

20. 6. 2026

Étoiles | Étoiles massives de la séquence principale

Image: HD 48914 binary system characteristics measured via photometric and radial velocity data

HD 48914 is an eclipsing binary system where the Be-shell star spins at its physical limit of 467 km/s. New data from TESS reveals a large surrounding gas disk and confirms the companion star was previously stripped of its mass through intense stellar interaction....

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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.

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.

More about Étoiles

Random terms

Position de la étoile Luminosité Température des étoiles Masse stellaire Taille de l´étoile L´âge des étoiles

	HD 37356 1484 ly			Discovery of the λ Bootis phenomenon in an early B-type star 10. 8. 2026
	VOS 70 3810 ly			A λ=1.3 millimeter Survey for Disks around Herbig Be Stars 24. 6. 2026
	HD 48914 2673 ly			A Be-shell star rotating at the critical limit and a partially stripped companion in a post-mass-transfer solution for the eclipsing binary V505 Mon 20. 6. 2026
	HD 188101 1394 ly			HD 188101: A Spotted B Star with Abundance Anomalies 6. 3. 2026
	Beta Pictoris 64 ly			The multi-wavelength vertical structure of the archetypal β Pictoris debris disk 5. 3. 2026

Liste des Étoiles massives de la séquence principale