11 Canis Minoris

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11 Canis Minoris
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Canis Minor
Right ascension  07h 46m 16.20081s[1]
Declination +10° 46′ 05.7055″[1]
Apparent magnitude (V) 5.25[2]
Spectral type A1Vnn[3]
B−V color index 0.018±0.008[2]
Radial velocity (Rv)+28.0±4.2[4] km/s
Proper motion (μ) RA: −29.902[1] mas/yr
Dec.: −25.275[1] mas/yr
Parallax (π)10.4262 ± 0.2007[1] mas
Distance313 ± 6 ly
(96 ± 2 pc)
Absolute magnitude (MV)0.42[2]
Mass2.23[5] M
Radius2.5[6] R
Luminosity65.26[2] L
Surface gravity (log g)3.60[5] cgs
Temperature9,972±339[5] K
Age149[5] Myr
Other designations
11 CMi, NSV 3724, BD+11°1670, FK5 1201, GC 10463, HD 62832, HIP 37921, HR 3008, SAO 97224[7]
Database references

11 Canis Minoris is a single[8] star in the equatorial constellation of Canis Minor,[7] located around 313 light years away from the Sun.[1] It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 5.25.[2] This object is moving away from the Earth with a heliocentric radial velocity of +28 km/s,[4] having come to within 157 light-years some 2.35 million years ago.[2]

This is an A-type main-sequence star with a stellar classification of A1Vnn,[3] where the 'n' notation indicates (very) "nebulous" lines due to rapid rotation. However, Gray and Garrison (1987) found a class of A0.5 IVnn,[9] which would instead match an evolving subgiant star. It is a suspected variable star of unknown type;[10] this object is 149[5] million years old with 2.23[5] times the mass of the Sun and about 2.5[6] times the Sun's radius. It is radiating 65[2] times the Sun's luminosity from its photosphere at an effective temperature of 9,972 K.[5]


  1. ^ a b c d e f 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. ^ a b c d e f g 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.
  3. ^ a b 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. ^ a b Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv:1606.08053, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065.
  5. ^ a b c d e f g 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.
  6. ^ a b Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics (Third ed.), 367 (2): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451.
  7. ^ a b "11 CMi". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-02.
  8. ^ Eggleton, P. P.; Tokovinin, A. A. (September 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.
  9. ^ Gray, R. O.; Garrison, R. F. (December 1987), "The Early A-Type Stars: Refined MK Classification, Confrontation with Stroemgren Photometry, and the Effects of Rotation", Astrophysical Journal Supplement, 65: 581, Bibcode:1987ApJS...65..581G, doi:10.1086/191237.
  10. ^ Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S.