Astronomy:Gliese 877
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Octans |
| Right ascension | 22h 55m 45.513s[1] |
| Declination | −75° 27′ 31.20″[1] |
| Apparent magnitude (V) | 10.377[2] |
| Characteristics | |
| Spectral type | M3V[3] |
| Astrometry | |
| Radial velocity (Rv) | +65.52±0.13[1] km/s |
| Proper motion (μ) | RA: −1,026.203[1] mas/yr Dec.: −1,059.407[1] mas/yr |
| Parallax (π) | 116.3134 ± 0.0168[1] mas |
| Distance | 28.041 ± 0.004 ly (8.597 ± 0.001 pc) |
| Absolute magnitude (MV) | 10.700 ± 0.0240[4] |
| Details[4] | |
| Radius | 0.442 ± 0.040 R☉ |
| Temperature | 3467 ± 100 K |
| Rotational velocity (v sin i) | 0.95 km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Gliese 877 (GJ 877 / HIP 113229 / LHS 531)[2] is a red dwarf star located in the southern constellation of Octans, near the boundary with Indus. At a distance of 28.04 light-years (8.60 parsecs), it is the nearest star in Octans.[5]: 84 Known stars close to it are β Hydri and ζ Tucanae, respectively 4.5 and 6.2 light years.[6]
Gliese 877's bolometric luminosity is just 2.3% of the Sun's.[7] It shines with an apparent magnitude of +10.22, so it cannot be seen with the naked eye. Nevertheless, it is considerably brighter than other red dwarfs, such as Proxima Centauri, the closest red dwarf to the Solar System; in particular, it is almost 14 times more luminous than Proxima. Of spectral type M3V,[3] its effective temperature is 3390 K.[7] It does not appear to be a variable star.[3]
See also
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 LHS 531 -- High proper-motion Star (SIMBAD)
- ↑ 3.0 3.1 3.2 Koen, C.; Kilkenny, D.; van Wyk, F.; Marang, F. (2010). "UBV(RI)C JHK observations of Hipparcos-selected nearby stars". Monthly Notices of the Royal Astronomical Society 403 (4): 1949–1968. doi:10.1111/j.1365-2966.2009.16182.x. pp. 1949-1968. Bibcode: 2010MNRAS.403.1949K.
- ↑ 4.0 4.1 Houdebine, E. R.; Mullan, D. J.; Paletou, F.; Gebran, M. (2016). "Rotation-Activity Correlations in K and M Dwarfs. I. Stellar Parameters and Compilations of v sin I and P/sin I for a Large Sample of Late-K and M Dwarfs". The Astrophysical Journal 822 (2): 97. doi:10.3847/0004-637X/822/2/97. Bibcode: 2016ApJ...822...97H.
- ↑ Kirkpatrick, J. Davy et al. (April 2024). "The Initial Mass Function Based on the Full-sky 20 pc Census of ~3600 Stars and Brown Dwarfs". The Astrophysical Journal Supplement Series 271 (2): 55. doi:10.3847/1538-4365/ad24e2. Bibcode: 2024ApJS..271...55K.
- ↑ "Stars within 15 light-years of Luyten 49-19 (The Internet Stellar Database)". http://www.stellar-database.com/Scripts/find_neighbors.exe?ID=157100&ly=15.
- ↑ 7.0 7.1 Morales, J. C.; Ribas, I.; Jordi, C. (2008). "The effect of activity on stellar temperatures and radii". Astronomy and Astrophysics 478 (2): 507–512. doi:10.1051/0004-6361:20078324. pp. 507-512. Bibcode: 2008A&A...478..507M.
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