CL Draconis

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CL Draconis
Quadrans muralis map.png
Red circle.svg
CL Draconis (circled), with the obsolete constellation Quadrans Muralis in the background.
Observation data
Epoch J2000       Equinox J2000
Constellation Draco
Right ascension 15h 57m 47.44180s [1]
Declination +54° 44′ 59.1428″ [1]
Apparent magnitude  (V)4.96 [2]
Characteristics
Spectral type F0 IV [3]
B−V color index 0.269±0.008 [2]
Variable type δ Sct [4]
Astrometry
Radial velocity (Rv)−11.0±4.2 [5]  km/s
Proper motion (μ)RA: −151.643 [1]   mas/yr
Dec.: +107.519 [1]   mas/yr
Parallax (π)29.9305 ± 0.1368  mas [1]
Distance 109.0 ± 0.5  ly
(33.4 ± 0.2  pc)
Absolute magnitude  (MV)2.33 [2]
Details
Mass 1.68±0.01 [6]   M☉
Luminosity 10.2+0.2
−0.3 [6]   L☉
Surface gravity (log g)4.04±0.14 [7]   cgs
Temperature 7,439±253 [7]   K
Metallicity [Fe/H]0.04±0.10 [8]   dex
Rotational velocity (v sin i)165 [6]  km/s
Age 643 [7]   Myr
Other designations
CL Dra, AG+54° 1023, BD+55° 1793, FK5  595, HD  143466, HIP  78180, HR  5960, SAO  29727 [9]
Database references
SIMBAD data

CL Draconis is a single [10] star in the northern circumpolar constellation of Draco. It can be viewed with the naked eye, having an apparent visual magnitude of 4.96. [2] The distance to this star, as determined from its annual parallax shift of 29.9  mas , [1] is 109  light years. It is moving closer to the Earth with a heliocentric radial velocity of −11 km/s. [5] The star has a relatively high proper motion, traversing the celestial sphere at the rate of 0.185″ /yr. [11]

Based upon a stellar classification of F0 IV, [3] this is an aging F-type subgiant star that has consumed the hydrogen at its core. It is spinning rapidly with a projected rotational velocity of 165 km/s, [6] giving it an oblate shape with an equatorial bulge that is estimated to be 8% larger than the polar radius. [12]

caption=Visual band light curves for CL Draconis, adapted from DuPuy and Burgoyne (1983) CLDraLightCurve.png
caption=Visual band light curves for CL Draconis, adapted from DuPuy and Burgoyne (1983)

CL Draconis is a Delta Scuti variable, changing brightness with an amplitude of 0.010 magnitude over a period of 1.83 hours. [14] CL Dra has 1.68 [6] times the mass of the Sun and is radiating 10.2 [6] times the Sun's luminosity from its photosphere at an effective temperature of 7,439 K. [7]

It was transferred from Draco to Quadrans Muralis. Later when the International Astronomical Union officially recognised constellations, Quadrans Muralis became obsolete, so this star was moved back to Draco.

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References

  1. 1 2 3 4 5 6 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 .
  2. 1 2 3 4 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. 1 2 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.
  4. ↑ Samus', N. N; Kazarovets, E. V; Durlevich, O. V; Kireeva, N. N; Pastukhova, E. N (2017), "General catalogue of variable stars: Version GCVS 5.1", Astronomy Reports, 61 (1): 80, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID   125853869.
  5. 1 2 de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv: 1208.3048 , Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID   59451347, A61.
  6. 1 2 3 4 5 6 Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv: 1201.2052 , Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID   55586789
  7. 1 2 3 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, arXiv: 1501.03154 , Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID   33401607.
  8. ↑ Gáspár, András; et al. (August 2016), "The Correlation between Metallicity and Debris Disk Mass", The Astrophysical Journal, 826 (2): 14, arXiv: 1604.07403 , Bibcode:2016ApJ...826..171G, doi: 10.3847/0004-637X/826/2/171 , S2CID   119241004, 171.
  9. ↑ "CL Dra". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 3 September 2018.
  10. ↑ 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, arXiv: 0806.2878 , Bibcode:2008MNRAS.389..869E, doi: 10.1111/j.1365-2966.2008.13596.x , S2CID   14878976.
  11. ↑ Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal, 129 (3): 1483–1522, arXiv: astro-ph/0412070 , Bibcode:2005AJ....129.1483L, doi:10.1086/427854, S2CID   2603568.
  12. ↑ 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.
  13. ↑ DuPuy, D. L.; Burgoyne, L. G. (January 1983). "HR 5960: new observations and period search". Publications of the Astronomical Society of the Pacific. 95: 61–68. Bibcode:1983PASP...95...61D. doi: 10.1086/131118 . S2CID   127849050.
  14. ↑ Rodríguez, E.; et al. (June 2000), "A revised catalogue of δ Sct stars", Astronomy and Astrophysics Supplement, 144 (3): 469–474, Bibcode:2000A&AS..144..469R, doi: 10.1051/aas:2000221 , hdl: 10261/226673 .
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