Astronomy:HD 21278

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Short description: Binary star system in the constellation Perseus
HD 21278
Perseus constellation map.svg
Red circle.svg
Location of HD 21278 (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Perseus
Right ascension  03h 28m 03.07229s[1]
Declination 49° 03′ 46.3315″[1]
Apparent magnitude (V) 4.99[2]
Characteristics
Spectral type B5V[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: +21.784[1] mas/yr
Dec.: −26.036[1] mas/yr
Parallax (π)5.6334 ± 0.2298[1] mas
Distance580 ± 20 ly
(178 ± 7 pc)
Absolute magnitude (MV)−1.49[6]
Orbit[7]
Period (P)21.695±0.004 d
Semi-major axis (a)≥6.72 Gm
Eccentricity (e)0.12±0.04
Periastron epoch (T)24,446,714.5±0.2
Argument of periastron (ω)
(secondary)
109±3°
Semi-amplitude (K1)
(primary)
22.7±0.9 km/s
Semi-amplitude (K2)
(secondary)
49±3 km/s
Details
A
Mass4.597[8] M
Radius3.9[9] R
Luminosity940[6] L
Surface gravity (log g)4.152±0.113[10] cgs
Temperature15,274±244[10] K
Metallicity [Fe/H]0.00[11] dex
Rotational velocity (v sin i)75[10] km/s
Age187[11] or 60[6] Myr
Other designations
BD+48°920, GC 4108, HD 21278, HIP 16147, HR 1034, SAO 38849[12]
Database references
SIMBADdata

HD 21278 is a binary star[7] system in the constellation Perseus, located within the 60±7[6] million year old Alpha Persei Cluster.[7] 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 580 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.[13] It is a double-lined spectroscopic binary with an orbital period of 21.7 days and an eccentricity of 0.12.[7]

The primary component is a B-type main-sequence star with a stellar classification of B5V,[3] indicating it is generating energy through core hydrogen fusion. The star is spinning with a projected rotational velocity of 75 km/s.[10] It has 4.6[8] times the mass of the Sun and about 3.9[9] times the Sun's radius. HD 21278 is radiating 940[6] times the luminosity of the Sun from its photosphere at an effective temperature of 15,274 K.[10]

References

  1. 1.0 1.1 1.2 1.3 1.4 1.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. 2.0 2.1 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode2012AstL...38..331A.  Vizier catalog entry
  3. 3.0 3.1 Zuckerman, B. et al. (June 2012). "Stellar Membership and Dusty Debris Disks in the α Persei Cluster". The Astrophysical Journal 752 (1): 12. doi:10.1088/0004-637X/752/1/58. 58. Bibcode2012ApJ...752...58Z. 
  4. 4.0 4.1 Mallama, A. (2014). "Sloan Magnitudes for the Brightest Stars". The Journal of the American Association of Variable Star Observers 42 (2): 443. Bibcode2014JAVSO..42..443M. Vizier catalog entry
  5. 5.0 5.1 Pourbaix, D. et al. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics 424 (2): 727–732. doi:10.1051/0004-6361:20041213. Bibcode2004A&A...424..727P. 
  6. 6.0 6.1 6.2 6.3 6.4 Silaj, J.; Landstreet, J. D. (2014). "Accurate age determinations of several nearby open clusters containing magnetic Ap stars". Astronomy & Astrophysics 566: A132. doi:10.1051/0004-6361/201321468. Bibcode2014A&A...566A.132S. 
  7. 7.0 7.1 7.2 7.3 Morrell, Nidia; Abt, Helmut A. (July 10, 1992). "Spectroscopic binaries in the Alpha Persei cluster". Astrophysical Journal, Part 1 393 (2): 666–673. doi:10.1086/171534. Bibcode1992ApJ...393..666M. 
  8. 8.0 8.1 Sheikhi, Najmeh et al. (March 2016). "The binary fraction and mass segregation in Alpha Persei open cluster". Monthly Notices of the Royal Astronomical Society 457 (1): 1028–1036. doi:10.1093/mnras/stw059. Bibcode2016MNRAS.457.1028S. 
  9. 9.0 9.1 Pasinetti Fracassini, L. E. et al. (2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)". Astronomy & Astrophysics 367 (2): 521–24. doi:10.1051/0004-6361:20000451. Bibcode2001A&A...367..521P. 
  10. 10.0 10.1 10.2 10.3 10.4 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. doi:10.1088/0004-637X/804/2/146. Bibcode2015ApJ...804..146D. 
  11. 11.0 11.1 Gontcharov, G. A. (2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters 38 (12): 771–782. doi:10.1134/S1063773712120031. Bibcode2012AstL...38..771G. 
  12. "HD 21278". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+21278. 
  13. Struve, O. (December 1925). "Twelve new spectroscopic binaries". Astrophysical Journal 62: 434. doi:10.1086/142944. Bibcode1925ApJ....62..434S.