HR 5256
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| Observation data Epoch 2000 Equinox 2000 | |
|---|---|
| Constellation | Ursa Major |
| Right ascension | 13h 57m 32.0575s[1] |
| Declination | +61° 29′ 34.301″[1] |
| Apparent magnitude (V) | 6.520[2] |
| Characteristics | |
| Spectral type | K3 V[3] |
| U−B color index | 0.98[4] |
| B−V color index | 1.01[4] |
| Variable type | None |
| Astrometry | |
| Radial velocity (Rv) | −25.3[5] km/s |
| Proper motion (μ) | RA: −32.32[1] mas/yr Dec.: +216.49[1] mas/yr |
| Parallax (π) | 98.97 ± 0.56[1] mas |
| Distance | 33.0 ± 0.2 ly (10.10 ± 0.06 pc) |
| Absolute magnitude (MV) | 6.85 |
| Details | |
| Mass | 0.800[6] M☉ |
| Radius | 0.78[6] R☉ |
| Surface gravity (log g) | 4.54[7] cgs |
| Temperature | 4,843[7] K |
| Metallicity | [Fe/H] = 0.17[7] |
| Other designations | |
HR 5256 is a solitary, K-type main sequence star located thirty-three light-years away in the constellation Ursa Major. It has an estimated 80% of the Sun's mass and 78% of the Sun's radius.[6] The space velocity components of this star are (U, V, W) = (−2, −10, −25) km/s.[4] HR 5256 will make its closest approach to the Sun in about 333,000 ± 16,000 years, when it will be at a distance of 3.9 ± 0.2 parsecs.[9]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Perryman, M. A. C.; et al. (July 1997). "The HIPPARCOS Catalogue". Astronomy & Astrophysics 323: L49–L52. Bibcode:1997A&A...323L..49P.
- ↑ Oja, T. (August 1991). "UBV photometry of stars whose positions are accurately known. VI". Astronomy and Astrophysics Supplement Series 89 (2): 415–419. Bibcode:1991A&AS...89..415O.
- ↑ Marrese, P. M.; Boschi, F.; Munari, U. (August 2003). "High resolution spectroscopy over lambda lambda 8500-8750 Å for GAIA. IV. Extending the cool MK stars sample". Astronomy and Astrophysics 406: 995–999. Bibcode:2003A&A...406..995M. doi:10.1051/0004-6361:20030647.
- ↑ 4.0 4.1 4.2 "ARICNS 4C04262". ARICNS. Astronomisches Rechen-Institut Heidelberg. March 4, 1998. Retrieved 2010-12-07.
- ↑ Wilson, Ralph Elmer (1953). General Catalogue of Stellar Radial Velocities. Washington: Carnegie Institution of Washington. Bibcode:[http://adsabs.harvard.edu/abs/1953QB901.W495..... 1953QB901.W495.....]
- ↑ 6.0 6.1 6.2 Takeda, Genya; et al. (February 2007). "Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog". The Astrophysical Journal Supplement Series 168 (2): 297–318. arXiv:astro-ph/0607235. Bibcode:2007ApJS..168..297T. doi:10.1086/509763. Data obtained from a VizieR query.
- ↑ 7.0 7.1 7.2 Soubiran, C.; Bienaymé, O.; Mishenina, T. V.; Kovtyukh, V. V. (March 2008). "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants". Astronomy and Astrophysics 480 (1): 91–101. arXiv:0712.1370. Bibcode:2008A&A...480...91S. doi:10.1051/0004-6361:20078788.
- ↑ "G 239-8 -- High proper-motion Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-12-07.
- ↑ García-Sánchez, J.; et al. (November 2001). "Stellar encounters with the solar system". Astronomy and Astrophysics 379: 634–659. Bibcode:2001A&A...379..634G. doi:10.1051/0004-6361:20011330.
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