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21 Canum Venaticorum

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Star in the constellation Canes Venatici
21 Canum Venaticorum
Observation data
Epoch J2000      Equinox J2000
Constellation Canes Venatici
Right ascension 13 18 14.50967
Declination +49° 40′ 55.4245″
Apparent magnitude (V) +5.14
Characteristics
Spectral type B9 IV (Si) or A0 V Si:
B−V color index −0.049±0.002
Variable type α CVn
Astrometry
Radial velocity (Rv)−2.9±2.8 km/s
Proper motion (μ) RA: −35.235 mas/yr
Dec.: +16.655 mas/yr
Parallax (π)11.7559 ± 0.1344 mas
Distance277 ± 3 ly
(85.1 ± 1.0 pc)
Absolute magnitude (MV)0.48
Details
Mass2.73 M
Radius2.8±0.3 R
Luminosity72.49 L
Surface gravity (log g)4.05 cgs
Temperature11,036±375 K
Rotational velocity (v sin i)96 km/s
Age201 Myr
Other designations
21 CVn, BK Canum Venaticorum, BD+50° 1994, FK5 3063, HD 115735, HIP 64906, HR 5023, SAO 44556
Database references
SIMBADdata

21 Canum Venaticorum is a single variable star in the northern constellation of Canes Venatici, located 277 light years away from the Sun. This object has the variable star designation BK Canum Venaticorum; 21 Canum Venaticorum is the Flamsteed designation. It is visible to the naked eye as a faint white-hued star with a baseline apparent visual magnitude of +5.14.

According to Garrison et al. (1994) this is a B-type subgiant star with a stellar classification of B9 IV (Si), where the suffix notation indicates this is a Silicon star. Cowley et al. (1969) listed it with a class of A0 V Si:, which would match an A-type main-sequence star with the ':' indicating some uncertainty in the classification. It is a marginally chemically-peculiar star with weaker than normal helium absorption lines and displaying helium line variability. The widths of the lines of ionized silicon vary with a period of 21.12 ± 0.48 hours.

21 Canum Venaticorum is classified as an Alpha Canum Venaticorum type variable star and its brightness varies by 0.04 magnitudes over a period of 18.4 hours. Its variability was discovered in 1984 by Juraj Zverko and it was given its variable star designation in 1987. It is around 201 million years old and is spinning with a relatively high projected rotational velocity of 96 km/s. The star has 2.73 times the mass of the Sun and 2.8 times the Sun's radius. It is radiating 72 times the luminosity of the Sun from its photosphere at an effective temperature of 11,036 K.

References

  1. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ 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.
  3. ^ Garrison, R. F; Gray, R. O (1994), "The late B-type stars: Refined MK classification, confrontation with stromgren photometry, and the effects of rotation", The Astronomical Journal, 107: 1556, Bibcode:1994AJ....107.1556G, doi:10.1086/116967.
  4. ^ Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819.
  5. ^ Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869, retrieved 2019-01-27.
  6. ^ North, P. (June 1998), "Do SI stars undergo any rotational braking?", Astronomy and Astrophysics, 334: 181–187, arXiv:astro-ph/9802286, Bibcode:1998A&A...334..181N
  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. "21 CVn". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-27.
  9. Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  10. Zverko, J.; et al. (March 1994), "Abundance Determination in the Chemically Peculiar Cp-Star 21-CANUM-VENATICORUM by Means of Spectrum Synthesis", Astronomy and Astrophysics, 283 (3): 932, Bibcode:1994A&A...283..932Z.
  11. Zverko, J. (September 1984), "Classification of Ap-Stars HR 830 and 21 CVn", Bulletin of the Astronomical Institute of Czechoslovakia, 35: 294, Bibcode:1984BAICz..35..294Z.
  12. Sriraghavan, S. M.; Jayakumar, K.; Babu, G. S. D.; Sajutha, S. (June 2004), "Variation of the Si II features in the chemically peculiar star - HD 115735", Bulletin of the Astronomical Society of India, 32 (2): 113, Bibcode:2004BASI...32..113S.
  13. Zverko, J. (September 1984). "Classification of Ap-Stars HR 830 and 21 CVn". Bulletin of the Astronomical Institute of Czechoslovakia. 35: 294–299. Bibcode:1984BAICz..35..294Z. Retrieved 28 August 2024.
  14. Kholopov, P. N.; Samus, N. N.; Kazarovets, E. V.; Kireeva, N. N. (August 1987). "The 68th Name-List of Variable Stars". Information Bulletin on Variable Stars. 3058 (3058): 1. Bibcode:1987IBVS.3058....1K. Retrieved 28 August 2024.
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