Loading
  • 21 Aug, 2019

  • By, Wikipedia

HD 133002

HD 133002 (HR 5596) is a possible binary star in the northern constellation of Ursa Minor. With an apparent visual magnitude of 5.65, 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° 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. If it was instead positioned at a distance of 33 ly (10 pc), this would be a second magnitude star. The system is drifting closer with a heliocentric radial velocity of −44 km/s.

This is a G-type main sequence star with a stellar classification of G2V, although it has also been classified as F9V or G0V. 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.

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

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

References

  1. ^ 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. ^ 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. ^ 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. ^ 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. ^ 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. ^ 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. ^ 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. ^ 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, vol. 1, Cambridge University Press, 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.