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HD 21278

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HD 21278
Location of HD 21278 (circled)
Observation data
Epoch J2000      Equinox ICRS
Constellation Perseus
Right ascension 03h 28m 03.07076s[1]
Declination +49° 03′ 46.3258″[1]
Apparent magnitude (V) 4.99[2]
Characteristics
Evolutionary stage Main sequence[3]
Spectral type B5V + B9V[3]
U−B color index −0.56[4]
B−V color index −0.10[4]
Astrometry
Radial velocity (Rv)+1.20[5] km/s
Proper motion (μ) RA: +22.754 mas/yr[1]
Dec.: −25.649 mas/yr[1]
Parallax (π)5.6775±0.1248 mas[1]
Distance570 ± 10 ly
(176 ± 4 pc)
Absolute magnitude (MV)−1.49[6]
Orbit[3]
Period (P)21.685415±0.000035 days
Semi-major axis (a)1.75820±0.00377 mas
Eccentricity (e)0.13843±0.00010
Inclination (i)148.938±0.030°
Longitude of the node (Ω)85.725±0.049°
Periastron epoch (T)mJD 46714.031±0.022
Argument of periastron (ω)
(secondary)		89.946±0.049°
Semi-amplitude (K1)
(primary)		31.45±0.31 km/s
Semi-amplitude (K2)
(secondary)		50.47±0.31 km/s
Details[3]
A
Mass5.381±0.084 M☉
Radius3.75±0.09 R☉
Luminosity940[6] L☉
Surface gravity (log g)4.152±0.113[7] cgs
Temperature16,750 K
Metallicity [Fe/H]0.00[8] dex
Rotational velocity (v sin i)53 km/s
Age49.5±6.0 Myr
B
Mass3.353±0.064 M☉
Temperature11,120 K
Age49.5±6.0 Myr
Other designations
BD+48°920, GC 4108, HD 21278, HIP 16147, HR 1034, SAO 38849[9]
Database references
SIMBADdata

HD 21278 is a binary star[10] system in the constellation Perseus, located within the Alpha Persei Cluster.[10] It has a blue-white hue and is visible to the naked eye with a combined apparent visual magnitude of 4.99.[2] The system is located at a distance of approximately 570 light years from the Sun based on parallax,[1] and it is drifting further away with a radial velocity of +1.20 km/s.[5]

The binary nature of this star was announced in 1925 by Otto Struve.[11] It is a double-lined spectroscopic binary with an orbital period of 21.685 days and an eccentricity of 0.138.[3]

The primary component is a B-type main-sequence star with a stellar classification of B5V, indicating it is generating energy through core hydrogen fusion. The star is spinning with a projected rotational velocity of 53 km/s. It has 5.381 times the mass of the Sun and about 3.75 times the Sun's radius.[3] HD 21278 A is radiating 940 times the luminosity of the Sun[6] from its photosphere at an effective temperature of 16,410 K.[3]

The secondary component is also a B-type main-sequence star, with a spectral class B9V. It has 3.353 times the mass of the Sun and an effective temperature of 11,120 K.[3]

References

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  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b 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. Vizier catalog entry
  3. ^ a b c d e f g h Danner, Christopher A.; Sandquist, Eric L.; Schaefer, Gail H.; Bedin, Luigi R.; Farrington, Christopher D.; Lanthermann, Cyprien; Kraus, Stefan; Klement, Robert; Anugu, Narsireddy (2025-06-09). "Precise Age For The Binary HD 21278 In The Young Alpha Persei Cluster". The Astrophysical Journal. arXiv:2506.08241v1. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213.
  4. ^ a b Mallama, A. (2014). "Sloan Magnitudes for the Brightest Stars". The Journal of the American Association of Variable Star Observers. 42 (2): 443. Bibcode:2014JAVSO..42..443M.Vizier catalog entry
  5. ^ a b Pourbaix, D.; et al. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics. 424 (2): 727–732. arXiv:astro-ph/0406573. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213. S2CID 119387088.
  6. ^ a b c Silaj, J.; Landstreet, J. D. (2014). "Accurate age determinations of several nearby open clusters containing magnetic Ap stars". Astronomy & Astrophysics. 566: A132. arXiv:1407.4531. Bibcode:2014A&A...566A.132S. doi:10.1051/0004-6361/201321468. S2CID 53370832.
  7. ^ David, Trevor J.; Hillenbrand, Lynne A. (2015). "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146. arXiv:1501.03154. Bibcode:2015ApJ...804..146D. doi:10.1088/0004-637X/804/2/146. S2CID 33401607.
  8. ^ Gontcharov, G. A. (2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters. 38 (12): 771–782. arXiv:1606.08814. Bibcode:2012AstL...38..771G. doi:10.1134/S1063773712120031. S2CID 118345778.
  9. ^ "HD 21278". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-12-16.
  10. ^ a b Morrell, Nidia; Abt, Helmut A. (July 10, 1992). "Spectroscopic binaries in the Alpha Persei cluster". Astrophysical Journal, Part 1. 393 (2): 666–673. Bibcode:1992ApJ...393..666M. doi:10.1086/171534.
  11. ^ Struve, O. (December 1925). "Twelve new spectroscopic binaries". Astrophysical Journal. 62: 434. Bibcode:1925ApJ....62..434S. doi:10.1086/142944.