HD 133002 Latitude and Longitude:

Sky map 14h 50m 20s, +82° 30′ 43″
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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]
Spectral type G2V [3]
U−B color index +0.17 [4]
B−V color index +0.671±0.004 [2]
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]
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

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 an 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]


  1. ^ a b c d e f g h i j Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. arXiv: 2208.00211. doi: 10.1051/0004-6361/202243940. Gaia DR3 record for this source at VizieR.
  2. ^ a b 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. ^ a b c 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. ^ a b 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. ^ a b c d 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. ^ 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. S2CID  56118016.
  7. ^ a b c 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. ^ a b c 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.