HD 21071
In today's world, HD 21071 has become a topic of great relevance and interest to a large number of people. Whether due to its impact on society, its historical relevance or its importance in the scientific field, HD 21071 has captured the attention of experts and enthusiasts alike. In this article we will explore in depth the most relevant aspects of HD 21071, analyzing its impact in various areas and its evolution over time. From its origins to its current state, we will embark on an exciting journey to deeply understand everything HD 21071 has to offer.
| 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 | 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]
| ID | Frequency (d−1) |
V Amplitude (mmag) |
Radial Velocity (km/s) |
|---|---|---|---|
| 1 | 1.18843 | 18.5 | 3.28±0.85 |
| 2 | 1.14934 | 7.7 | – |
| 3 | 1.41968 | 3.8 | – |
| 4 | 0.95706 | 3.0 | – |
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]
References
- ^ "Light Curve", Hipparcos ESA, ESA, retrieved 19 September 2022.
- ^ a b c d e 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.
- ^ a b c d 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.
- ^ a b c d e f g h i j k 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.
- ^ a b c d e f g h 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.
- ^ a b 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.
- ^ a b 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.
- ^ "HD 21071". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved October 26, 2018.
- ^ 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.
- ^ 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.
