Étoiles massives de la séquence principale

	Mass	Distance
Iota Leonis Ab GJ 11625, Gliese 11625		-	77 ly
Alpha Coronae Borealis Gemma, Alphecca, Ashtaroth, Gnosia Stella Coronae, 5 CrB, BD +27°2512, GCTP 3519.00, FK5 578, HD 139006, HIP 76267, HR 5793, SAO 83893	A1IV	2.6 M☉	77.2 ly
Omega Draconis ome Dra, ω Dra, 28 Dra, BD+68° 949, GJ 4017, HD 160922, HIP 86201, HR 6596, SAO 17576	F4V	1.5 M☉	77.5 ly
HD 214953 CD-4714307，SAO 231257，HR 8635	F9.5V	-	77.7 ly
12 Persei 12 Per, BD+39° 610, FK5 2187, GJ 105.6 АВ, Gliese 105.6 АВ, HD 16739, HIP 12623, HR 788, SAO 55793	F9V	1.4 M☉	78 ly
HD 49095	F6.5V	1.2 M☉	78.1 ly
Alpha1 Librae	F3V	1.4 M☉	78.1 ly
Kappa Phoenicis κ Phe, kap Phe, CD−44°101, GC 516, GJ 20, Gliese 20, HD 2262, HIP 2072, HR 100, SAO 215092	A5IVn	1.7 M☉	78.2 ly
37 Ceti WDS J01144-0755AB,	F5V	-	78.5 ly
HD 40397 TYC 4777-1763-1, HIP 28267, USNO-A2 0825-01805065	F7V	-	78.5 ly
HD 190422	F9VCH-0.4	-	78.6 ly
HD 76653 CPD−54° 1925, GJ 3519, Gliese 3519, HD 76653, HIP 43797, HR 3570, SAO 236405	F6V	1.2 M☉	79.4 ly
Zeta1 Cancri zet01 Cnc, Tegmine		-	79.8 ly
Zeta1 Cancri B		-	79.8 ly
HD 121560	F6V	-	79.9 ly
Delta Velorum Ab	A4V	2.3 M☉	80.6 ly
Delta Velorum B	F8V	1.4 M☉	80.6 ly
Zeta1 Ursae Majoris Ab	A2Vp	2.2 M☉	80.6 ly
Alcor g UMa, g Ursae Majoris, 80 Ursae Majoris, BD+55 1603, CCDM J13240+5456D, GC 18155, HD 116842, HIP 65477, HR 5062, PPM 34021, SAO 28751, WDS J13239+5456C	A5V	1.8 M☉	80.6 ly
HD 104731 TYC 7763-1047-1, USNO-A2 0450-13777979, HR 4600, HIP 58803, CD-41 6938，SAO 223193	F5V	-	80.7 ly

Nombre de la estrella

Mass

Distance

77 ly

Gemma, Alphecca, Ashtaroth, Gnosia Stella Coronae, 5 CrB, BD +27°2512, GCTP 3519.00, FK5 578, HD 139006, HIP 76267, HR 5793, SAO 83893

A1IV

2.6 M☉

77.2 ly

Omega Draconis

ome Dra, ω Dra, 28 Dra, BD+68° 949, GJ 4017, HD 160922, HIP 86201, HR 6596, SAO 17576

F4V

1.5 M☉

77.5 ly

HD 214953

CD-4714307，SAO 231257，HR 8635

F9.5V

77.7 ly

12 Persei

12 Per, BD+39° 610, FK5 2187, GJ 105.6 АВ, Gliese 105.6 АВ, HD 16739, HIP 12623, HR 788, SAO 55793

F9V

1.4 M☉

78 ly

HD 49095

F6.5V

1.2 M☉

78.1 ly

Alpha1 Librae

F3V

1.4 M☉

78.1 ly

Kappa Phoenicis

κ Phe, kap Phe, CD−44°101, GC 516, GJ 20, Gliese 20, HD 2262, HIP 2072, HR 100, SAO 215092

A5IVn

1.7 M☉

78.2 ly

37 Ceti

WDS J01144-0755AB,

F5V

78.5 ly

HD 40397

TYC 4777-1763-1, HIP 28267, USNO-A2 0825-01805065

F7V

78.5 ly

HD 190422

F9VCH-0.4

78.6 ly

HD 76653

CPD−54° 1925, GJ 3519, Gliese 3519, HD 76653, HIP 43797, HR 3570, SAO 236405

F6V

1.2 M☉

79.4 ly

79.8 ly

79.8 ly

F6V

79.9 ly

Delta Velorum Ab

A4V

2.3 M☉

80.6 ly

Delta Velorum B

F8V

1.4 M☉

80.6 ly

Zeta1 Ursae Majoris Ab

A2Vp

2.2 M☉

80.6 ly

Alcor

g UMa, g Ursae Majoris, 80 Ursae Majoris, BD+55 1603, CCDM J13240+5456D, GC 18155, HD 116842, HIP 65477, HR 5062, PPM 34021, SAO 28751, WDS J13239+5456C

A5V

1.8 M☉

80.6 ly

HD 104731

TYC 7763-1047-1, USNO-A2 0450-13777979, HR 4600, HIP 58803, CD-41 6938，SAO 223193

F5V

80.7 ly

Estrellas masivas de la secuencia principal noticias

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

10. 8. 2026

Estrellas | Estrellas masivas de la secuencia princi

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

Estrellas | Estrellas masivas de la secuencia principal | Formación planetari

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

Estrellas | Estrellas masivas de la secuencia princi

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.

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.

More about Estrellas

Random terms

Posición de la estrella Luminosidad Temperatura de la estrella Masa estelar Tamaño de la estrella Edad de las estrellas

	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

Lista de Étoiles massives de la séquence principale

Estrellas masivas de la secuencia principal noticias

Research in Étoiles massives de la séquence principale

Frequently Asked Questions about nearby stars

What is the nearest star?

What are the nearest stars to Earth?

What is the solar neighborhood?

How do astronomers measure distances to stars?

Are there any exoplanets orbiting the nearest stars?

Why are the nearest stars important for astronomy and physics?

StellarGuide: Estrellas