HD 21071

Last updated
HD 21071
V576PerLightCurve.png
A light curve for V576 Persei, plotted from Hipparcos data [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Perseus
Right ascension 03h 25m 57.382s [2]
Declination +49° 07′ 14.73″ [2]
Apparent magnitude  (V)6.09 [3]
Characteristics
Evolutionary stage Main sequence
Spectral type B7 V [4]
B−V color index −0.073±0.005 [3]
Variable type SPB [5]
Astrometry
Radial velocity (Rv)−1.5±0.9 [6]  km/s
Proper motion (μ)RA: +23.753  mas/yr [2]
Dec.: −26.656  mas/yr [2]
Parallax (π)6.0959 ± 0.0444  mas [2]
Distance 535 ± 4  ly
(164 ± 1  pc)
Absolute magnitude  (MV)−0.19 [3]
Details
Mass 3.69+0.14
−0.15 [5]   M☉
Radius 2.21 [7]   R☉
Luminosity 278.0+53.1
−44.7 [5]   L☉
Surface gravity (log g)4.30 [4]   cgs
Temperature 14,768 [4]   K
Metallicity [Fe/H]0.0082+0.0053
−0.0032 [5]   dex
Rotational velocity (v sin i)58 [4]  km/s
Age 90 [4]   Myr
Other designations
V576 Per, BD+48° 913, GC  4075, HD  21071, HIP  15988, HR  1029, SAO  38817 [8]
Database references
SIMBAD data

HD 21071 is a blue-white hued variable star in the northern constellation of Perseus. Also known as V576 Persei, it is a sixth magnitude star that is dimly visible to the naked eye under good viewing conditions, having an apparent visual magnitude of 6.09. [3] The brightness of the star varies with a multiperiodic cycle. [9] The distance to HD 21071, as determined from an annual parallax shift of 6.1  mas , [2] is 535  light years. It is a member of the young Alpha Persei cluster, Melotte 20, [4] [10] and moving is closer to the Earth with a heliocentric radial velocity of −1.5 km/s. [6]

This is a B-type main-sequence star with a stellar classification of B7 V. [4] HD 21071 belongs to an unusual stellar population termed 'sn' stars. These seem to be related to chemically peculiar stars, but have sharp ('s') Balmer and metal absorption lines with "broad coreless He I" ('n') lines. The latter wide, "nebulous" lines may be due to Stark broadening caused by an electric field. [4] HD 21071 is a slowly pulsating B-type star (SPB star) that was initially found to vary with a period of 0.84 days. Further study revealed four frequencies, with the two dominant, higher amplitude frequencies having similar cycles of 1.19 and 1.15 per day. [5]

Pulsation Periods [5]
ID Frequency
(d−1)		 V   Amplitude
(mmag)		Radial Velocity
(km/s)
11.1884318.53.28±0.85
21.149347.7–
31.419683.8–
40.957063.0–

Stellar models show the star to have 3.7 [5] times the mass of the Sun, with 2.21 [7] times the Sun's radius. It is 90 [4]  million years old with a near-solar metallicity and is spinning with a projected rotational velocity of 58 km/s. [4] The star is radiating 278 [5] times the Sun's luminosity from its photosphere at an effective temperature of 14,768 K. [4]

Related Research Articles

<span class="mw-page-title-main">28 Aquilae</span> Star in the constellation Aquila

28 Aquilae, abbreviated 28 Aql, is a star in the equatorial constellation of Aquila. 28 Aquilae is its Flamsteed designation though it also bears the Bayer designation A Aquilae, and the variable star designation V1208 Aquilae. It has an apparent visual magnitude is 5.5, making this a faint star that requires dark suburban skies to view. The annual parallax shift of 9.6 mas means this star is located at a distance of approximately 340 light-years from Earth.

3 Centauri is a triple star system in the southern constellation of Centaurus, located approximately 300 light years from the Sun. It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.32. As of 2017, the two visible components had an angular separation of 7.851″ along a position angle of 106°. The system has the Bayer designation k Centauri; 3 Centauri is the Flamsteed designation. It is a suspected eclipsing binary with a variable star designation V983 Centauri.

<span class="mw-page-title-main">V1472 Aquilae</span> Binary star system in the constellation Aquila

V1472 Aquilae is a triple star system in the equatorial constellation of Aquila. It is a variable star that ranges in brightness from 6.36 down to 6.60. The system is located at a distance of approximately 780 light years from the Sun based on parallax. It is a high-velocity star system with a radial velocity of −112 km/s.

<span class="mw-page-title-main">BX Boötis</span> Star in the constellation Boötes

BX Boötis is a star in the northern constellation of Boötes. It is a dim star near the lower limit of visibility to the naked eye, having a nominal apparent visual magnitude of 6.35. Based upon an annual parallax shift of 10.81 mas, it is located 302 light years away. At that distance, the visual magnitude of the star is diminished by an extinction of 0.13 due to interstellar dust. It is moving closer with a heliocentric radial velocity of −11 km/s.

<span class="mw-page-title-main">Psi Persei</span> Star in the constellation Perseus

Psi Persei is a single Be star in the northern constellation of Perseus. It has an apparent visual magnitude of about 4.2, so it is visible to the naked eye at night under suitably dark skies. Based on parallax measurements, it is located at a distance of roughly 580 light-years from the Earth.

<span class="mw-page-title-main">Epsilon Doradus</span> Star in the constellation Dorado

Epsilon Doradus, Latinzied from ε Doradus, is a solitary star located in the southern constellation of Dorado. It is visible to the naked eye with an apparent visual magnitude of 5.11. Based upon an annual parallax shift of 5.68 mas as measured from Earth, it is located roughly 570 light years from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.09 due to interstellar dust.

<span class="mw-page-title-main">53 Persei</span> Star in the constellation Perseus

53 Persei is a single variable star in the northern constellation of Perseus. It has the Bayer designation d Persei, while 53 Persei is the Flamsteed designation. The star is visible to the naked eye as a faint, blue-white hued point of light with an apparent visual magnitude of 4.80. It is located approximately 480 light years away from the Sun, as determined from parallax, and is drifting further away with a radial velocity of +7.3 km/s.

<span class="mw-page-title-main">4 Persei</span> Star in the constellation Perseus

4 Persei is a single star in the northern constellation of Perseus, located around 670 light years away from the Sun. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 5.04 The Bayer designation for this star is g Persei; 4 Persei is the Flamsteed designation. This object has a peculiar velocity of 26.3 km/s and may be a runaway star.

<span class="mw-page-title-main">HD 21278</span> Binary star system in the constellation Perseus

HD 21278 is a binary star system in the constellation Perseus, located within the 60±7 million year old Alpha Persei Cluster. It has a blue-white hue and is visible to the naked eye with a combined apparent visual magnitude of 4.99. The system is located at a distance of approximately 580 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +1.20 km/s.

30 Persei is a binary star system in the northern constellation Perseus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.49. Based upon an annual parallax shift of 4.46±0.39 mas, is located roughly 730 light years from the Sun. It is a member of the Perseus OB3 association, which includes the Alpha Persei Cluster.

<span class="mw-page-title-main">29 Persei</span> Star in the constellation Perseus

29 Persei is a single star in the northern constellation of Perseus, located approximately 640 light years away from the Sun based on parallax. It is visible to the naked eye as faint, blue-white hued star with an apparent visual magnitude of 5.16. This object is a member of the Alpha Persei Cluster.

<span class="mw-page-title-main">ET Virginis</span> Evolved red giant star in the constellation Virgo

ET Virginis is a single, red-hued star in the equatorial constellation of Virgo. It can be viewed with the naked eye, having an apparent visual magnitude of 4.91. Based upon an annual parallax shift of 5.9 mas, it is located 560 light years away. It is moving further from the Earth with a heliocentric radial velocity of +18.6 km/s, having come within 177 ly of the Sun around 6.3 million years ago.

<span class="mw-page-title-main">9 Persei</span> Blue supergiant star in the constellation Perseus

9 Persei is a single variable star in the northern constellation Perseus, located around 4,300 light years away from the Sun. It has the Bayer designation i Persei; 9 Persei is the Flamsteed designation. This body is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of about 5.2. It is moving closer to the Sun with a heliocentric radial velocity of −15.2 km/s. The star is a member of the Perseus OB1 association of co-moving stars.

57 Persei, or m Persei, is a suspected triple star system in the northern constellation of Perseus. It is at the lower limit of visibility to the naked eye, having a combined apparent visual magnitude of 6.08. The annual parallax shift of 16.4 mas provides a distance measure of 199 light years. 57 Persei is moving closer to the Sun with a radial velocity of about −23 km/s and will make perihelion in around 2.6 million years at a distance of roughly 22 ly (6.6 pc).

<span class="mw-page-title-main">42 Persei</span> Binary star system in the constellation Perseus

42 Persei is a binary star system in the northern constellation of Perseus. It has the Bayer designation n Persei, while 42 Persei is the Flamsteed designation. The system is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude of 5.11. It is located around 93 parsecs (302 ly) distant from the Sun, but is drifting closer with a radial velocity of −12.4 km/s.

<span class="mw-page-title-main">31 Persei</span> Star in the constellation Perseus

31 Persei is a single star in the northern constellation of Perseus. It is visible to the naked eye as a dim, blue-white hued point of light with an apparent visual magnitude of 5.05. This star is located around 172 parsecs (560 ly) away from the Sun, and it is drifting closer with a radial velocity of −1.6 km/s. It is likely a member of the Alpha Persei Cluster.

<span class="mw-page-title-main">21 Persei</span> Star in the constellation Perseus

21 Persei is a single, variable star in the northern constellation of Perseus, located about 331 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 5.10 km/s. The object is moving further from the Earth with a heliocentric radial velocity of +8.5 km/s. It has the variable star designation LT Persei; 21 Persei is the Flamsteed designation.

<span class="mw-page-title-main">55 Persei</span> Star in the constellation Perseus

55 Persei is a single, blue-white hued star in the northern constellation Perseus. It is faintly visible to the naked eye under good seeing conditions, having an apparent visual magnitude of 5.73. Based upon an annual parallax shift of 8.50±0.38 mas as seen from Earth's orbit, the star is located about 380 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction of 0.39 due to interstellar dust.

<span class="mw-page-title-main">BF Antliae</span> Star in the constellation Antlia

BF Antliae, or HD 86301, is a variable star in the southern constellation of Antlia. It has a baseline apparent visual magnitude of 6.32, which indicates it lies near the lower limit of visibility for faint stars. The distance to BF Ant, as determined from its annual parallax shift of 6.9 mas, is 473 light years. It is moving further away with a heliocentric radial velocity of +18 km/s.

<span class="mw-page-title-main">HD 118285</span> SPB star in the constellation Chamaeleon.

HD 118285, also known as HR 5115, is a variable star located in the southern circumpolar constellation Chamaeleon. DY Chamaeleontis is its variable star designation. It has an average apparent magnitude of 6.32, placing it near the limit for naked eye visibility. The object is located relatively far at a distance of 864 light years based on Gaia DR3 parallax measurements but is receding with a heliocentric radial velocity of 18 km/s. At its current distance, HD 118285's brightness is diminished by 0.58 magnitudes due to interstellar dust.

References

  1. ↑ "Light Curve", Hipparcos ESA, ESA, retrieved 19 September 2022.
  2. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  3. 1 2 3 4 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971 , Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID   119257644.
  4. 1 2 3 4 5 6 7 8 9 10 11 Saffe, C.; Levato, H. (February 2014), "On the nature of sn stars. I. A detailed abundance study", Astronomy & Astrophysics, 562: 17, arXiv: 1401.5764 , Bibcode:2014A&A...562A.128S, doi:10.1051/0004-6361/201322091, S2CID   119261402, A128.
  5. 1 2 3 4 5 6 7 8 Szewczuk, W.; Daszyńska-Daszkiewicz, J. (October 2015), "Seismic modelling of the rotating, slowly pulsating B-type star HD 21071", Monthly Notices of the Royal Astronomical Society, 453 (1): 277–286, arXiv: 1507.03609 , Bibcode:2015MNRAS.453..277S, doi:10.1093/mnras/stv1589.
  6. 1 2 Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv: 1606.08053 , Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID   119231169.
  7. 1 2 Mathias, P.; et al. (December 2001), "Spectroscopic monitoring of 10 new northern slowly pulsating B star candidates discovered from the HIPPARCOS mission" (PDF), Astronomy and Astrophysics, 379 (3): 905–916, Bibcode:2001A&A...379..905M, doi: 10.1051/0004-6361:20011406 .
  8. ↑ "HD 21071". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved October 26, 2018.
  9. ↑ Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, GCVS 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID   125853869.
  10. ↑ Zuckerman, B.; et al. (June 2012), "Stellar Membership and Dusty Debris Disks in the α Persei Cluster", The Astrophysical Journal, 752 (1): 12, arXiv: 1204.3950 , Bibcode:2012ApJ...752...58Z, doi:10.1088/0004-637X/752/1/58, S2CID   119207634, 58.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.