14 Comae Berenices
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Coma Berenices |
| Right ascension | 12h 26m 24.06442s[1] |
| Declination | +27° 16′ 05.6598″[1] |
| Apparent magnitude (V) | 4.95[2] |
| Characteristics | |
| Evolutionary stage | subgiant[1] |
| Spectral type | F0p[3][4] |
| U−B color index | +0.18[2] |
| B−V color index | +0.277±0.018[5] |
| Astrometry | |
| Radial velocity (Rv) | −2.20[6] km/s |
| Proper motion (μ) | RA: −15.874[1] mas/yr Dec.: −11.784[1] mas/yr |
| Parallax (π) | 11.2826±0.1085 mas[1] |
| Distance | 289 ± 3 ly (88.6 ± 0.9 pc) |
| Absolute magnitude (MV) | +0.35[7] |
| Details | |
| Mass | 1.6[8] M☉ |
| Radius | 4.8[8] R☉ |
| Luminosity | 56[8] L☉ |
| Surface gravity (log g) | 3.27[8] cgs |
| Temperature | 7,170[8] K |
| Rotation | 1.272 days[9] |
| Rotational velocity (v sin i) | 226[7] km/s |
| Age | 500[1] Myr |
| Other designations | |
| 14 Com, AAVSO 1221+27, BD+28°2115, FK5 2997, HD 108283, HIP 60697, HR 4733, SAO 82310[10] | |
| Database references | |
| SIMBAD | data |
14 Comae Berenices is a single[3] star in the northern constellation of Coma Berenices, and is the second brightest[11] member of the Coma Star Cluster.[3] It is a faint star but visible to the naked eye with an apparent visual magnitude of 4.95.[2] Parallax measurements place the star at a distance of about 289 light years.[1]
The spectrum of this star is peculiar and it has been assigned a number of different stellar classifications: A5, F0p, F0 III Sr, F0 vp,[3] F1 IV: np Sr shell,[5] A9 IV np Sr II,[12] F1 IV,[13] and A9 V + shell.[14] Abt & Morrell (1995) designated this a Lambda Boötis star but this was later refuted.[12] No surface magnetic field has been detected on 14 Comae Berenices.[15]
14 Comae Berenices is a well-known[14] shell star with a high rate of spin, showing a projected rotational velocity of 226 km/s.[7] This is giving the star an oblate shape with an equatorial bulge that is 12% larger than the polar radius.[4] It is radiating 56 times the Sun's luminosity from its photosphere at an effective temperature of 7,170 K.[8]
References
- ^ a b c d e f g h 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.
- ^ a b c Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
- ^ a b c d Abou Elazm, M. S. (October 1993), "The composite spectrum of the A type star 14 Comae", Astrophysics and Space Science, 208 (1): 1–4, Bibcode:1993Ap&SS.208....1A, doi:10.1007/BF00658127, S2CID 123520053
- ^ a b van Belle, Gerard T. (March 2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2, S2CID 119273474
- ^ 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.
- ^ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 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 c Pizzolato, N.; et al. (2000). "Evolution of X-ray activity of 1-3 Msun late-type stars in early post-main-sequence phases". Astronomy and Astrophysics. 361: 614. Bibcode:2000A&A...361..614P.
- ^ a b c d e f Stassun, Keivan G.; et al. (2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467.
- ^ Balona, L. A. (2022). "Rapidly oscillating TESS A-F main-sequence stars: Are the roAp stars a distinct class?". Monthly Notices of the Royal Astronomical Society. 510 (4): 5743. arXiv:2109.02246. Bibcode:2022MNRAS.510.5743B. doi:10.1093/mnras/stac011.
- ^ "14 Com". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-01-02.
- ^ Dominy, J. F.; Smith, M. A. (1977). "A spectroscopic study of 14 Comae and other A-type shell stars". Astrophysical Journal. 217: 494. Bibcode:1977ApJ...217..494D. doi:10.1086/155598.
- ^ a b Murphy, Simon J.; et al. (October 2015), "An Evaluation of the Membership Probability of 212 λ Boo Stars. I. A Catalogue", Publications of the Astronomical Society of Australia, 32: 43, arXiv:1508.03633, Bibcode:2015PASA...32...36M, doi:10.1017/pasa.2015.34, S2CID 59405545, e036
- ^ Gray, R. O.; et al. (2001). "The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars". The Astronomical Journal. 121 (4): 2148. Bibcode:2001AJ....121.2148G. doi:10.1086/319956.
- ^ a b Abt, Helmut A.; Willmarth, Daryl W. (August 1999), "Binaries in the Praesepe and Coma Star Clusters and Their Implications for Binary Evolution", The Astrophysical Journal, 521 (2): 682–690, Bibcode:1999ApJ...521..682A, doi:10.1086/307569, S2CID 119772785
- ^ Kudryavtsev, D. O.; et al. (November 2006). "New magnetic chemically peculiar stars". Monthly Notices of the Royal Astronomical Society. 372 (4): 1804–1828. Bibcode:2006MNRAS.372.1804K. doi:10.1111/j.1365-2966.2006.10994.x.