HD 133002
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Ursa Minor |
| Right ascension | 14h 50m 20.41906s[1] |
| Declination | +82° 30′ 42.9972″[1] |
| Apparent magnitude (V) | 5.65[2] |
| Characteristics | |
| Spectral type | F9 V[3] |
| U−B color index | +0.17[2] |
| B−V color index | +0.638[3] |
| Astrometry | |
| Radial velocity (Rv) | −44.38[3] km/s |
| Proper motion (μ) | RA: +176.85[1] mas/yr Dec.: −223.52[1] mas/yr |
| Parallax (π) | 23.10 ± 0.23 mas[1] |
| Distance | 141 ± 1 ly (43.3 ± 0.4 pc) |
| Absolute magnitude (MV) | 2.448[3] |
| Details | |
| HD 133002 A | |
| Mass | 1.51[4] M☉ |
| Surface gravity (log g) | 3.86[5] cgs |
| Temperature | 5,461[5] K |
| Metallicity [Fe/H] | −0.41[6] dex |
| Rotational velocity (v sin i) | 5.2[5] km/s |
| Age | 2.80[4] Gyr |
| HD 133002 B | |
| Mass | 0.15±0.01[7] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
| ARICNS | data |
HD 133002 (HR 5596) is a main sequence star in the northern constellation of Ursa Minor. With an apparent visual magnitude of 5.65,[2] it is faintly visible to the naked eye. (According to the Bortle scale, it can be viewed from dark rural skies.) The high declination of +82.5°[1] means it is hidden from view from most of the southern hemisphere. Parallax measurements made with the Hipparcos spacecraft yield an estimated distance of around 141 light years from the Sun.[1] If it was instead positioned at a distance of 33 ly (10 pc), this would be a second magnitude star.[3]
This is an F-type main sequence star with a stellar classification of F9 V.[3] It is estimated to have 51% greater mass than the Sun, and is younger with an age of around 2.8 billion years.[4] The projected rotational velocity along the star's equator is a relatively leisurely 5.2 km/s.[5] The star is considered a photometric solar analog, although it is deficient in elements more massive than helium when compared to the Sun.[9] The chemical composition and relatively low surface gravity for a star of its classification suggest that this may instead be a subgiant star that is in the process of evolving away from the main sequence.[10] The effective temperature of the star's photosphere is 5,461 K,[5] giving it the yellow-white hue of an F-type star.[11]
This star has been examined for evidence of an infrared excess, but none was detected.[12] During a 2006−2007 survey of nearby stars, it was discovered that HD 133002 has a low-mass common proper motion stellar companion. This object has an estimated 15% of the Sun's mass. It has a projected separation of around 80 AU from the primary, which suggests an orbital period of roughly 700 years. At present, there is insufficient observational data available to determine orbital elements.[7]
References
- ^ a b c d e f g van Leeuwen, F. (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 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M.
- ^ a b c d e f Soubiran, C.; et al. (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.
- ^ a b c Casagrande, L.; et al. (June 2011). "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey". Astronomy & Astrophysics. 530 (A138): 21. arXiv:1103.4651. Bibcode:2011A&A...530A.138C. doi:10.1051/0004-6361/201016276.
- ^ a b c d e Schröder, C.; et al. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo" (PDF), Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377.[permanent dead link]
- ^ 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.
- ^ a b Heinze, A. N.; et al. (May 2010), "Constraints on Long-period Planets from an L'- and M-band Survey of Nearby Sun-like Stars: Observations", The Astrophysical Journal, 714 (2): 1551–1569, arXiv:1003.5340, Bibcode:2010ApJ...714.1551H, doi:10.1088/0004-637X/714/2/1551.
- ^ "HD 133002". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-01-09.
{{cite web}}: CS1 maint: postscript (link) - ^ Bikmaev, I.; Galeev, A.; Sakhibullin, N.; Musaev, F. (2005), Hill, V.; François, P.; Primas, F. (eds.), "Chemical compositions of photometric solar-analog stars and F-G stars of different ages", From Lithium to Uranium: Elemental Tracers of Early Cosmic Evolution, IAU Symposium Proceedings of the international Astronomical Union 228, Held in Paris, France, May 23–27, 2005, vol. 1, Cambridge University Press, pp. 239–240, Bibcode:2005IAUS..228..239B, doi:10.1017/S1743921305005624.
- ^ Galeev, A. I.; et al. (June 2004), "Chemical Composition of 15 Photometric Analogues of the Sun", Astronomy Reports, 48 (6): 492–510, Bibcode:2004ARep...48..492G, doi:10.1134/1.1767216.
- ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 10, 2012, retrieved 2016-01-12.
- ^ 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.
