HD 133002

HD 133002 (HR 5596) is a possible binary[7] 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°[9] means it is hidden from view from most of the southern hemisphere. Parallax measurements yield an estimated distance of around 143 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]

HD 133002
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ursa Minor
Right ascension 14h 50m 20.42394s[1]
Declination +82° 30′ 42.9883″[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: +177.190[1] mas/yr
Dec.: −223.948[1] mas/yr
Parallax (π)22.8454 ± 0.1009[1] mas
Distance142.8 ± 0.6 ly
(43.8 ± 0.2 pc)
Absolute magnitude (MV)2.448[3]
Details
HD 133002 A
Mass1.51[4] M☉
Radius3.33+0.06
−0.13[1] R☉
Luminosity9.821±0.054[1] L☉
Surface gravity (log g)3.86[5] cgs
Temperature5,599+114
−46[1] K
Metallicity [Fe/H]−0.41[6] dex
Rotational velocity (v sin i)5.2[5] km/s
Age2.80[4] Gyr
HD 133002 B
Mass0.15±0.01[7] M☉
Other designations
BD+83°431, FK5 1644, GJ 3876, HD 133002, HIP 72573, HR 5596, SAO 2459[8]
Database references
SIMBADdata
ARICNSdata

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.[10] 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.[11] The effective temperature of the star's photosphere is 5,599 K,[1] giving it the yellow-white hue of an F-type star.[12]

This star has been examined for evidence of an infrared excess, but none was detected.[13] 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
  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  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.
  3. 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.
  4. 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.
  5. 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.
  6. 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.
  7. 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.
  8. "HD 133002". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-01-09.
  9. 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.
  10. 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, Cambridge University Press, 1, pp. 239–240, Bibcode:2005IAUS..228..239B, doi:10.1017/S1743921305005624.
  11. 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.
  12. "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.
  13. 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.

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