HD 133002
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ursa Minor
Right ascension 14h 50m 20.421s[1]
Declination +82° 30′ 42.99″[1]
Apparent magnitude (V) 5.63[2]
Characteristics
Spectral type G2V[3]
U−B color index +0.17[4]
B−V color index +0.671±0.004[2]
Astrometry
Radial velocity (Rv)−44.38[5] km/s
Proper motion (μ) RA: +177.593 mas/yr[1]
Dec.: −224.260 mas/yr[1]
Parallax (π)22.9030 ± 0.0496 mas[1]
Distance142.4 ± 0.3 ly
(43.66 ± 0.09 pc)
Absolute magnitude (MV)2.448[5]
Details
HD 133002 A
Mass1.51[6] M☉
Radius3.4[1] R☉
Luminosity9.54±0.04[1] L☉
Surface gravity (log g)3.86[7] cgs
Temperature5,515±1[1] K
Metallicity [Fe/H]−0.41[8] dex
Rotational velocity (v sin i)5.2[7] km/s
Age2.80[6] Gyr
HD 133002 B
Mass0.15±0.01[9] M☉
Other designations
BD+83°431, FK5 1644, GJ 3876, HD 133002, HIP 72573, HR 5596, SAO 2459[10]
Database references
SIMBADdata
ARICNSdata

HD 133002 (HR 5596) is a possible binary[9] star in the northern constellation of Ursa Minor. With an apparent visual magnitude of 5.65,[4] 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 yield an estimated distance of around 142 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.[5] The system is drifting closer with a heliocentric radial velocity of −44 km/s.[5]

This is a G-type main sequence star with a stellar classification of G2V,[3] although it has also been classified as F9V or G0V.[11] With spectral absorption lines of metals and absorption bands of some molecules weaker than expected based on its hydrogen lines, it is defined as a weak line star. Based on its G-band strengths, it would we given a class of G0, and based on its metal lines a class of G1.[3]

It is estimated to have 51% greater mass than the Sun, and is younger with an age of around 2.8 billion years.[6] The projected rotational velocity along the star's equator is a relatively leisurely 5.2 km/s.[7] The star is considered a photometric solar analog, although it is deficient in elements more massive than helium when compared to the Sun.[12] 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.[13] The effective temperature of the star's photosphere is 5,515 K,[1] giving it the yellow-white hue of a G-type star.[14]

This star has been examined for evidence of an infrared excess, but none was detected.[15] 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.[9]

References

  1. 1 2 3 4 5 6 7 8 9 10 11 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. 1 2 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  3. 1 2 3 Abt, Helmut A. (1986). "Spectral Classification of Weak-lined Stars Discovered Photometrically". The Astrophysical Journal. 309: 260. Bibcode:1986ApJ...309..260A. doi:10.1086/164597.
  4. 1 2 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M.
  5. 1 2 3 4 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, S2CID 16602121.
  6. 1 2 3 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. S2CID 56118016.
  7. 1 2 3 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.
  8. ↑ 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, S2CID 46328823.
  9. 1 2 3 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, S2CID 119199321.
  10. ↑ "HD 133002". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-01-09.{{cite web}}: CS1 maint: postscript (link)
  11. ↑ Skiff, B. A. (2014). "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009-2016)". VizieR On-line Data Catalog: B/Mk. Originally Published in: Lowell Observatory (October 2014). 1. Bibcode:2014yCat....1.2023S.
  12. ↑ Bikmaev, I.; et al. (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, Cambridge University Press, vol. 1, pp. 239–240, Bibcode:2005IAUS..228..239B, doi:10.1017/S1743921305005624.
  13. ↑ 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, S2CID 119473855.
  14. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2016-01-12.
  15. ↑ 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, S2CID 54940779.
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