Étoiles massives de la séquence principale

	Mass	Distance
HIP 99770 b03 Cyg, 29 Cygni, HD 192640, HR 7736, IRAS 20126+3639, 2MASS J20143203+3648225, SAO 69678, TIC 10988057, TYC 2683-3962-1, V1644 Cyg, WISEA J201432.07+364823.7	kA1.5hA7mA0.5 λ	1.9 M☉	133 ly
HD 206893 HIC 107412, HIP 107412, 2MASS J21452190-1246599, TIC 155782207, TYC 5796-1161-1, Gaia DR2 6843672087120107264	F5V C	1.2 M☉	133 ly
HR 8799 HD 218396, V342 Pegasi, BD+20 5278, FK5 3850, GC 32209, HIP 114189, PPM 115157, SAO 91022, TYC 1718-2350-1	F0+VkA5mA5 C	1.6 M☉	133 ly
Achernar 2 G. Eri, α Eri, 70 Eri, CD−57°334, FK5 54, HD 10144, HIP 7588, HR 472, SAO 232481, 水委一	B3 Vpe	6 M☉	139 ly
Achernar B	A1V-A3V	2 M☉	139 ly
HIP 1481 HD 1466, 2MASS J00182612-6328389, 1RXS J001826.2-632837, SAO 248159, TIC 425934574, TYC 8843-1330-1, WISEA J001826.27-632839.6	F8V C	1.2 M☉	140 ly
HIP 21152 HD 28992, HIP 21152, TYC 1266-278-1	F5V	1.4 M☉	141 ly
HD 57625 HIP 36014	F8	1 M☉	145 ly
TOI 554		1.3 M☉	147 ly
HD 984	F7V	1.2 M☉	149 ly
HD 143105	F5	1.5 M☉	152 ly
HD 181327	F5/6	1.4 M☉	156 ly
Eta Telescopii η Tel, Eta Tel, CPD−54° 9339, HD 181296, HIP 95261, HR 7329, SAO 246055	A0 Vn	3.2 M☉	158 ly
HD 32115	A9	-	160 ly
HIP 88399 HD 164249, IRAS 17591-5139, 2MASS J18030341-5138564, TIC 337438474, TYC 8369-1619-1, UCAC4 192-178768	F6V C	1.3 M☉	161 ly
HIP 11696 HD 15407		-	161 ly
HD 62364	F7V	-	173 ly
HIP 63734	F7/8V	1.2 M☉	176 ly
HD 103891	F8V	1.3 M☉	179 ly
HD 129209 HD 129209		1.1 M☉	179 ly

Nombre de la estrella

Mass

Distance

b03 Cyg, 29 Cygni, HD 192640, HR 7736, IRAS 20126+3639, 2MASS J20143203+3648225, SAO 69678, TIC 10988057, TYC 2683-3962-1, V1644 Cyg, WISEA J201432.07+364823.7

kA1.5hA7mA0.5 λ

1.9 M☉

133 ly

HD 206893

HIC 107412, HIP 107412, 2MASS J21452190-1246599, TIC 155782207, TYC 5796-1161-1, Gaia DR2 6843672087120107264

F5V C

1.2 M☉

133 ly

HR 8799

HD 218396, V342 Pegasi, BD+20 5278, FK5 3850, GC 32209, HIP 114189, PPM 115157, SAO 91022, TYC 1718-2350-1

F0+VkA5mA5 C

1.6 M☉

133 ly

Achernar

2 G. Eri, α Eri, 70 Eri, CD−57°334, FK5 54, HD 10144, HIP 7588, HR 472, SAO 232481, 水委一

B3 Vpe

6 M☉

139 ly

Achernar B

A1V-A3V

2 M☉

139 ly

HIP 1481

HD 1466, 2MASS J00182612-6328389, 1RXS J001826.2-632837, SAO 248159, TIC 425934574, TYC 8843-1330-1, WISEA J001826.27-632839.6

F8V C

1.2 M☉

140 ly

HIP 21152

HD 28992, HIP 21152, TYC 1266-278-1

F5V

1.4 M☉

141 ly

HD 57625

HIP 36014

1 M☉

145 ly

TOI 554

1.3 M☉

147 ly

HD 984

F7V

1.2 M☉

149 ly

HD 143105

1.5 M☉

152 ly

HD 181327

F5/6

1.4 M☉

156 ly

Eta Telescopii

η Tel, Eta Tel, CPD−54° 9339, HD 181296, HIP 95261, HR 7329, SAO 246055

A0 Vn

3.2 M☉

158 ly

HD 32115

160 ly

HIP 88399

HD 164249, IRAS 17591-5139, 2MASS J18030341-5138564, TIC 337438474, TYC 8369-1619-1, UCAC4 192-178768

F6V C

1.3 M☉

161 ly

HIP 11696

HD 15407

161 ly

HD 62364

F7V

173 ly

HIP 63734

F7/8V

1.2 M☉

176 ly

HD 103891

F8V

1.3 M☉

179 ly

HD 129209

1.1 M☉

179 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