Astronomy:21 Canum Venaticorum
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Canes Venatici |
| Right ascension | 13h 18m 14.50967s[1] |
| Declination | +49° 40′ 55.4245″[1] |
| Apparent magnitude (V) | +5.14[2] |
| Characteristics | |
| Spectral type | B9 IV (Si)[3] or A0 V Si:[4] |
| B−V color index | −0.049±0.002[2] |
| Variable type | α2 CVn[5] |
| Astrometry | |
| Radial velocity (Rv) | −2.9±2.8[2] km/s |
| Proper motion (μ) | RA: −35.235[1] mas/yr Dec.: +16.655[1] mas/yr |
| Parallax (π) | 11.7559 ± 0.1344[1] mas |
| Distance | 277 ± 3 ly (85.1 ± 1.0 pc) |
| Absolute magnitude (MV) | 0.48[6] |
| Details | |
| Mass | 2.73[7] M☉ |
| Radius | 2.8±0.3[6] R☉ |
| Luminosity | 72.49[2] L☉ |
| Surface gravity (log g) | 4.05[7] cgs |
| Temperature | 11,036±375[7] K |
| Rotational velocity (v sin i) | 96[7] km/s |
| Age | 201[7] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
21 Canum Venaticorum is a single[9] variable star[5] in the northern constellation of Canes Venatici, located 277 light years away from the Sun.[1] 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.[2]
According to Garrison et al. (1994)[3] 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:,[4] which would match an A-type main-sequence star with the ':' indicating some uncertainty in the classification. It is a marginally chemically-peculiar star[10] with weaker than normal helium absorption lines and displaying helium line variability.[11] The widths of the lines of ionized silicon vary with a period of 21.12 ± 0.48 hours.[12]
21 Canum Venaticorum is classified as an Alpha2 Canum Venaticorum type variable star and its brightness varies by 0.04 magnitudes over a period of 18.4 hours.[5] It is around 201 million years old and is spinning with a relatively high projected rotational velocity of 96 km/s.[7] The star has 2.73[7] times the mass of the Sun and 2.8[6] times the Sun's radius. It is radiating 72[2] times the luminosity of the Sun from its photosphere at an effective temperature of 11,036 K.[7]
References
- ↑ 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. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 3.0 3.1 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, doi:10.1086/116967, Bibcode: 1994AJ....107.1556G.
- ↑ 4.0 4.1 Cowley, A. et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal 74: 375–406, doi:10.1086/110819, Bibcode: 1969AJ.....74..375C.
- ↑ 5.0 5.1 5.2 Samus, N. N. et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1 61 (1): 80–88, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S, http://www.sai.msu.su/gcvs/gcvs/, retrieved 2019-01-27.
- ↑ 6.0 6.1 6.2 North, P. (June 1998), "Do SI stars undergo any rotational braking?", Astronomy and Astrophysics 334: 181–187, Bibcode: 1998A&A...334..181N
- ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 7.7 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, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D.
- ↑ "21 CVn". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=21+CVn.
- ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ 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.
- ↑ 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.
- ↑ 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.
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