10 Canum Venaticorum
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Canes Venatici |
| Right ascension | 12h 44m 59.40506s[1] |
| Declination | +39° 16′ 44.1061″[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: –359.87[1] mas/yr Dec.: +140.16[1] mas/yr |
| Parallax (π) | 57.55 ± 0.32[1] mas |
| Distance | 56.7 ± 0.3 ly (17.38 ± 0.10 pc) |
| Details | |
| Surface gravity (log g) | 4.29[2] cgs |
| Temperature | 5,789[2] K |
| Metallicity [Fe/H] | –0.53[2] dex |
| Rotational velocity (v sin i) | 8.11[5] km/s |
| Age | 6.3[2] Gyr |
| Other designations | |
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 0.05755 arc seconds as measured by the Hipparcos satellite,[1] this system is 56.7 light-years (17.38 parsecs) from Earth.
The stellar classification of 10 Canum Venaticorum is G0 V,[2] indicating that it is a main sequence star that is fusing hydrogen into helium at its core to generate energy. It is older than the Sun, with an estimated age of six billion years.[2] The effective temperature of the stellar atmosphere is 5,789 K,[2] giving it the yellow hue of a G-type star.[7]
An excess of infrared emission at a wavelength of 70 μm suggests the presence of a debris disk. A temperature of 94 K indicates that this dusty disk is orbiting at a distance of about 12 AU from the host star.[8]
References
- 1 2 3 4 5 6 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.
- 1 2 3 4 5 6 7 8 9 10 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.
- 1 2 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.
- ↑ 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.
- ↑ 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", Astronomy and Astrophysics 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725.
- ↑ "10 CVn -- High proper-motion Star", SIMBAD Astronomical Database (Centre de Données astronomiques de Strasbourg), retrieved 2014-01-26.
- ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, retrieved 2012-01-16.
- ↑ 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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