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Étoiles massives de la séquence principale
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Liste des Étoiles massives de la séquence principale

        
    
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Etoile 41-60
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Nom de l étoile Mass Distance

19 Draconis
BD+65° 1157, Gliese 648, GJ 648, HD 153597, HIP 82860, HR 6315, SAO 17281, h Draconis
F8V 1 M☉ 50 ly

WG 21
DA6.6 - 50.2 ly

Castor Aa
Alpha Geminorum, α Gem, 66 Geminorum, FK5 287, GJ 278, Gliese 278, HIP 36850, SAO 60198, BD+32°1581A, PLX 1785.00, HR 2891, HD 60179
A1V 2.8 M☉ 50.9 ly

Castor Ba
BD+32°1581B, HR 2890, HD 60178
A2Vm 3 M☉ 50.9 ly

Sigma Boötis
* sig Boo, σ Boo, 28 Boötis, BD+30°2536, GC 19659, Gliese 557, GJ 557, HD 128167, HIP 71284, HR 5447, SAO 83416, CCDM 14347+2945
F4VkF2mF1 1.2 M☉ 51.4 ly

99 Herculis
b Her, 99 Her, BD+30°3128, GJ 704, HD 165908, HIP 88745, HR 6775, SAO 66648
F7VgF7mF5 0.94 M☉ 51.4 ly

Chi Herculis
chi Her, χ Her, 1 Her, BD+42° 2648, FK5 1166, Gliese 602, GJ 602, HD 142373, HIP 77760, HR 5914, SAO 45772, WDS J16254+1402AB
F8VFe-2Hdel-1 1.1 M☉ 51.9 ly

Phi2 Ceti
phi02 Cet, φ2 Cet, 19 Cet, NSV 316, BD−11° 153, GJ 37, Gliese 37, HD 4813, HIP 3909, HR 235, SAO 147470
F7V 1.2 M☉ 51.9 ly

10 Ursae Majoris
10 UMa, 10 UMa, BD+42° 1956, FK5 339, Gliese 332, GJ 332, HD 76943, HIP 44248, HR 3579, SAO 42642
F3V 1.4 M☉ 52.4 ly

HD 65907
LHS 1959, GCRV 5309, IDS 07559-6002 A, PPM 356380, CCDM J07578-6018A, LFT 560, SAO 250035, CD -59 1773, GJ 294 A, Gliese 294, LPM 276, Ci 20 453, HD 65907A, LTT 3020, SPOCS 359, 2MASS J07574692-6018111, TD1 11543, CPC 20.1 2000, HIC 38908, NLTT 18763, TYC 8911-793-1, CPD -59 944, HIP 38908, PLX 1902, UBV 7701, GC 10804, HR 3138, PM 07569-6010, uvby98 225160124
F9.5V 0.91 M☉ 52.7 ly

I Carinae
I Car, CD−73° 576, GJ 391, Gliese 391, HD 90589, HIC 50954, HIP 50954, HR 4102, SAO 256710
F3V 1.4 M☉ 53.1 ly

Alpha Circini
17. G Circini, CD−64° 86, HD 128898, HIP 71908, HR 5463, SAO 252853, alf Cir
A7VpSrCrEu 1.6 M☉ 53.5 ly

Ksi Pegasi
ksi Peg, LHS 3851, GJ 872, Gliese 872
F6V 1.2 M☉ 53.5 ly

Psi5 Aurigae
psi05 Aur, 56 Aurigae, ADS 5425, BD+43°1595, FK5 255, GJ 245, Gliese 245, HD 48682, HIP 32480, HR 2483, SAO 41330
F9V 1.1 M☉ 54.2 ly

HD 55575
HR 2721, HIP 35136, GJ 1095, Gliese 1095, SAO 41644, BD+47 1419, TYC 3396-2196-1
F9V 0.91 M☉ 55 ly

58 Ophiuchi
58 Oph, BD−21°4712, FK5 1463, GC 24030, Gliese 692, GJ 692, HD 160915, HIP 86736, HR 6595, SAO 185660, Gaia EDR3 4117290138348536064
F5V 1.3 M☉ 56 ly

HD 10647
q01 Eri, q1 Eridani, 5 G. Eridani, Gliese 3109, GJ 3109, HR 506, HIC 7978, HIP 7978, SAO 232501, CPD−54° 365, WISE J014229.49-534428.1, TIC 229137615, TYC 8475-527-1, 2MASS J01422932-5344271
F9V 1.1 M☉ 56.6 ly

Iota Horologii
ι Hor, GJ 108, Gliese 108, HD 17051, HIC 12653, HIP 12653, HR 810, 2MASS J02423346-5048008, LTT 1322, NLTT 8800, TIC 166853853, TYC 8056-1164-1, WISEA J024233.84-504758.7
F8V C 1.3 M☉ 56.6 ly

g Lupi
CD−44° 10310, CPD−44° 7529, GC 21070, GJ 594, Gliese 594, HD 139664, HIP 76829, HR 5825, SAO 226064, PPM 320883, LTT 6256, NLTT 40843
F3/5V 1.4 M☉ 56.7 ly

Xi Ophiuchi
ksi Oph, ξ Oph, 40 Ophiuchi, BD−20°4731, FK5 917, GC 23423, HD 156897, HIP 84893, HR 6445, SAO 185296, CCDM J17210-2107AB, WDS J17210-2107AB, LTT 6908
F2V 1.3 M☉ 57.1 ly
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Étoiles massives de la séquence principale nouvelles

Lambda Bootis phenomenon identified in the massive early B-type star HD 37356
icon10. 8. 2026
iconÉtoiles | 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
icon24. 6. 2026
iconÉtoiles | 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
icon20. 6. 2026
iconÉtoiles | 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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study iconResearch in Étoiles massives de la séquence principale

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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: 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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