10_Canum_Venaticorum

10 Canum Venaticorum

10 Canum Venaticorum

Star in the constellation Canes Venatici

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 faintly seen with the naked eye from suburban locations. Based upon an annual parallax shift of 0.057 arcseconds,[1] this system is 57.26 light-years (17.557 parsecs) from Sun. It is drifting further away with a radial velocity of +80 km/s.[4]

Quick Facts Observation data Epoch J2000 Equinox J2000, Constellation ...

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,[10] 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%[7] 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.[8] 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,[7] giving it the yellow hue of a G-type star.[11]

An excess of infrared emission at a wavelength of 70 μm suggests the presence of a debris disk.[12] 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. [1]
    Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. [2]
    Maldonado, J.; et al. (May 2012), "Metallicity of solar-type stars with debris discs and planets", Astronomy and Astrophysics, 541: A40, arXiv:1202.5884, Bibcode:2012A&A...541A..40M, doi:10.1051/0004-6361/201218800, S2CID 46328823.
  3. [3]
    Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
  4. [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, S2CID 11027621.
  5. [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, S2CID 119232172, A114.
  6. [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. S2CID 119199829.
  7. [7]
    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.
  8. [8]
    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, S2CID 43455849, archived from the original (PDF) on 2017-09-22, retrieved 2018-11-04.
  9. [9]
    "10 CVn -- High proper-motion Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2014-01-26.
  10. [10]
    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. S2CID 119476992.
  11. [11]
    "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16.
  12. [12]
    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, S2CID 54940779.
Share this article:

This article uses material from the Wikipedia article 10_Canum_Venaticorum, and is written by contributors. Text is available under a CC BY-SA 4.0 International License; additional terms may apply. Images, videos and audio are available under their respective licenses.