Étoiles massives de la séquence principale

	Mass	Distance
* 17 Vir	F8V	-	97.9 ly
* 47 Oph	F3V	-	98.1 ly
HD 63008	F9VFe-0.5	-	98.1 ly
HD 125987	A0V	-	98.1 ly
HD 18387	F5V	-	98.1 ly
HD 120237	F9V	-	98.2 ly
HD 209635	F8V	-	98.2 ly
HD 63332	F6V	-	98.3 ly
HD 88955 q Velorum, CD−41° 5713, FK5 382, GC 14076, HD 88955, HIP 50191, HR 4023, SAO 221895	A2 V	2.2 M☉	99.7 ly
Lambda Boötis Xuange, λ Boo, 19 Boötis, BD+46°1949, FK5 527, GC 19273, GJ 3837, Gliese 3837, HD 125162, HIP 69732, HR 5351, SAO 44965	A0p λB	1.7 M☉	100 ly
HD 167665	F9VFe-0.8CH-0.4	-	101 ly
HD 50554 BD+24°1451, GC 9043, HIP 33212, SAO 78855, GSC 01894-01961, TOI-6965	F8V	1.1 M☉	102 ly
Alkaid Eta Ursae Majoris, Benetnash, Benetnasch, Elkeid, η UMa, 85 UMa, BD+50°2027, FK5 509, GC 18643, HD 120315, HIC 67301, HIP 67301, HR 5191, PPM 53742, SAO 44752	B3 V	6.1 M☉	104 ly
HR 858 HD 17926, CD-31 1148, GC 3443, HIC 13363, HIP 13363, 2MASS J02515623-3048524, TIC 178155732, TOI-396, TYC 7012-833-1	F6V C	1.1 M☉	104 ly
HR 2562 HD 50571	F5VFe+0.4	1.3 M☉	111 ly
HD 196885 HIP 101966, HR 7907, 2MASS J20395188+1114588, TIC 282257777, TYC 1092-1778-1, YZ 11 8063	F8V C	1.3 M☉	111 ly
HD 73344 TIC 175193677, BD+24 1968, FK5 4776, HIP 42403, 2MASS J08384552+2341094, TYC 1942-1827-1, WISEA J083845.48+234107.7, EPIC 212178066	F6V C	1.2 M☉	115 ly
HD 55693 HIP 34879		-	119 ly
HD 7449 BD−05 215, HIP 5806, TYC 4683-883-1, 2MASS J01142933-0502504	F9.5V	1.1 M☉	126 ly
HIP 560 HD 203, HR 9	F2V	1.5 M☉	130 ly

Nombre de la estrella

Mass

Distance

* 17 Vir

F8V

97.9 ly

* 47 Oph

F3V

98.1 ly

HD 63008

F9VFe-0.5

98.1 ly

HD 125987

A0V

98.1 ly

HD 18387

F5V

98.1 ly

HD 120237

F9V

98.2 ly

HD 209635

F8V

98.2 ly

HD 63332

F6V

98.3 ly

HD 88955

q Velorum, CD−41° 5713, FK5 382, GC 14076, HD 88955, HIP 50191, HR 4023, SAO 221895

A2 V

2.2 M☉

99.7 ly

Lambda Boötis

Xuange, λ Boo, 19 Boötis, BD+46°1949, FK5 527, GC 19273, GJ 3837, Gliese 3837, HD 125162, HIP 69732, HR 5351, SAO 44965

A0p λB

1.7 M☉

100 ly

HD 167665

F9VFe-0.8CH-0.4

101 ly

HD 50554

BD+24°1451, GC 9043, HIP 33212, SAO 78855, GSC 01894-01961, TOI-6965

F8V

1.1 M☉

102 ly

Alkaid

Eta Ursae Majoris, Benetnash, Benetnasch, Elkeid, η UMa, 85 UMa, BD+50°2027, FK5 509, GC 18643, HD 120315, HIC 67301, HIP 67301, HR 5191, PPM 53742, SAO 44752

B3 V

6.1 M☉

104 ly

HR 858

HD 17926, CD-31 1148, GC 3443, HIC 13363, HIP 13363, 2MASS J02515623-3048524, TIC 178155732, TOI-396, TYC 7012-833-1

F6V C

1.1 M☉

104 ly

HR 2562

HD 50571

F5VFe+0.4

1.3 M☉

111 ly

HD 196885

HIP 101966, HR 7907, 2MASS J20395188+1114588, TIC 282257777, TYC 1092-1778-1, YZ 11 8063

F8V C

1.3 M☉

111 ly

HD 73344

TIC 175193677, BD+24 1968, FK5 4776, HIP 42403, 2MASS J08384552+2341094, TYC 1942-1827-1, WISEA J083845.48+234107.7, EPIC 212178066

F6V C

1.2 M☉

115 ly

HD 55693

HIP 34879

119 ly

HD 7449

BD−05 215, HIP 5806, TYC 4683-883-1, 2MASS J01142933-0502504

F9.5V

1.1 M☉

126 ly

HIP 560

HD 203, HR 9

F2V

1.5 M☉

130 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