Gliese 673
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Ophiuchus |
| Right ascension | 17h 25m 45.23266s[1] |
| Declination | +02° 06′ 41.1208″[1] |
| Apparent magnitude (V) | 7.492[2] |
| Characteristics | |
| Spectral type | K7V[2] |
| U−B color index | 1.261[2] |
| B−V color index | 1.373[2] |
| Astrometry | |
| Radial velocity (Rv) | −24.4[3] km/s |
| Proper motion (μ) | RA: −579.66[1] mas/yr Dec.: −1,184.76[1] mas/yr |
| Parallax (π) | 129.86 ± 0.73 mas[1] |
| Distance | 25.1 ± 0.1 ly (7.70 ± 0.04 pc) |
| Absolute magnitude (MV) | 8.06[2] |
| Details | |
| Radius | 0.564[4] R☉ |
| Surface gravity (log g) | 4.70[5] cgs |
| Temperature | 4,030[4] K |
| Metallicity [Fe/H] | −0.20[5] dex |
| Rotation | 11.94 days[6] |
| Age | (205 ± 21) × 106[6] years |
| Other designations | |
| Database references | |
| SIMBAD | data |
Gliese 673 is an orange dwarf star in the constellation Ophiuchus. It has a stellar classification of K7V.[2] Main sequence stars with this spectra have a mass in the range of 60-70% of solar mass (M☉) (comparable to the members of the binary star system 61 Cygni).
This star is relatively near our Sun at a distance of about 25 light years. In spite of this proximity, however, it is still too faint to be viewed by the unaided eye. It is considered a slowly rotating star with a relatively high proper motion.
See also
References
- ^ a b c d e 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
- ^ a b c d e f Koen, C.; et al. (April 2010), "UBV(RI)C JHK observations of Hipparcos-selected nearby stars", Monthly Notices of the Royal Astronomical Society, 403 (4): 1949–1968, Bibcode:2010MNRAS.403.1949K, doi:10.1111/j.1365-2966.2009.16182.x
{{citation}}: CS1 maint: unflagged free DOI (link) - ^ 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
- ^ a b van Belle, Gerard T.; von Braun, Kaspar (April 2009), "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars", The Astrophysical Journal, 694 (2): 1085–1098, arXiv:0901.1206, Bibcode:2009ApJ...694.1085V, doi:10.1088/0004-637X/694/2/1085
- ^ a b Frasca, A.; et al. (December 2009), "REM near-IR and optical photometric monitoring of pre-main sequence stars in Orion. Rotation periods and starspot parameters", Astronomy and Astrophysics, 508 (3): 1313–1330, arXiv:0911.0760, Bibcode:2009A&A...508.1313F, doi:10.1051/0004-6361/200913327
- ^ a b Barnes, Sydney A. (November 2007), "Ages for Illustrative Field Stars Using Gyrochronology: Viability, Limitations, and Errors", The Astrophysical Journal, 669 (2): 1167–1189, arXiv:0704.3068, Bibcode:2007ApJ...669.1167B, doi:10.1086/519295
- ^ "LHS 447 -- High proper-motion Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2011-10-15
External links
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