10 Canum Venaticorum

10 Canum Venaticorum is the Flamsteed designation for an ordinary star in the northern constellation of Canes Venatici. It has an apparent visual magnitude of 5.95,[2] which, according to the Bortle scale, can be seen with the naked eye from suburban locations. Based upon an annual parallax shift of 0.0569 arcseconds,[1] this system is 57.3 light-years (17.57 parsecs) from Sun. It is drifting further away with a radial velocity of +80 km/s.[4]

10 Canum Venaticorum
Observation data
Epoch J2000      Equinox J2000
Constellation Canes Venatici
Right ascension 12h 44m 59.40507s[1]
Declination +39° 16′ 44.0983″[1]
Apparent magnitude (V) 5.95[2]
Characteristics
Spectral type G0 V[2]
U−B color index –0.03[3]
B−V color index +0.55[3]
Astrometry
Radial velocity (Rv)+80.3[4] km/s
Proper motion (μ) RA: –359.785[1] mas/yr
Dec.: +138.994[1] mas/yr
Parallax (π)56.9309 ± 0.0730[1] mas
Distance57.29 ± 0.07 ly
(17.57 ± 0.02 pc)
Absolute magnitude (MV)4.76[5]
Details
Mass0.87+0.04
−0.03[6] M☉
Radius0.98±0.02[1] R☉
Luminosity1.104±0.002[1] L☉
Surface gravity (log g)4.29[2] cgs
Temperature5,968+58
−41[1] K
Metallicity [Fe/H]–0.53[2] dex
Rotation13 days[5]
Rotational velocity (v sin i)8.11[7] km/s
Age6.3[2] Gyr
Other designations
10 CVn, BD+40°2570, GJ 484, HD 110897, HIP 62207, HR 4845, SAO 63177[8]
Database references
SIMBADdata

The stellar classification of 10 Canum Venaticorum is G0 V,[2] indicating that it is a G-type main sequence star that is fusing hydrogen into helium at its core to generate energy. The NStars project found a similar class of F9V Fe−0.3,[9] indicating a mild underabundance of iron. It is older than the Sun, with an estimated age of six billion years.[2] The star has around 98%[1] of the Sun's radius and 87%[6] of the solar mass. It rotates about the axis an average of once every 13 days,[5] with a projected rotational velocity along the equator of 8 km/s.[7] The abundance of elements other than hydrogen and helium is lower than in the Sun.[2] The effective temperature of the stellar atmosphere is 5,968 K,[1] giving it the yellow hue of a G-type star.[10]

An excess of infrared emission at a wavelength of 70 μm suggests the presence of a debris disk.[11] The best fit disk model suggest a broad dust annulus with a peak brightness at a radius of 53.7 AU, that is inclined by an angle of 56° to the line of sight from the Earth along a position angle of 111.2°.[5]

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. Maldonado, J.; et al. (May 2012), "Metallicity of solar-type stars with debris discs and planets", Astronomy and Astrophysics, 541, arXiv:1202.5884, Bibcode:2012A&A...541A..40M, doi:10.1051/0004-6361/201218800.
  3. Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99), Bibcode:1966CoLPL...4...99J.
  4. Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14,000 F and G dwarfs", Astronomy and Astrophysics, 418: 989–1019, arXiv:astro-ph/0405198, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959.
  5. Marshall, J. P.; et al. (October 2014), "Interpreting the extended emission around three nearby debris disc host stars", Astronomy & Astrophysics, 570: 13, arXiv:1408.5649, Bibcode:2014A&A...570A.114M, doi:10.1051/0004-6361/201424517, A114.
  6. Ramírez, I.; et al. (September 2012). "Lithium Abundances in nearby FGK Dwarf and Subgiant Stars: Internal Destruction, Galactic Chemical Evolution, and Exoplanets". The Astrophysical Journal. 756 (1): 46. arXiv:1207.0499. Bibcode:2012ApJ...756...46R. doi:10.1088/0004-637X/756/1/46.
  7. Martínez-Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter" (PDF), Astronomy and Astrophysics, 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725.
  8. "10 CVn -- High proper-motion Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2014-01-26.
  9. Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637.
  10. "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 10, 2012, retrieved 2012-01-16.
  11. Trilling, D. E.; et al. (February 2008), "Debris Disks around Sun-like Stars", The Astrophysical Journal, 674 (2): 1086–1105, arXiv:0710.5498, Bibcode:2008ApJ...674.1086T, doi:10.1086/525514.
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