Kappa1 Lupi
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Lupus
Right ascension 15h 11m 56.07286s[1]
Declination −48° 44′ 16.1692″[1]
Apparent magnitude (V) 3.86[2]
Characteristics
Spectral type B9.5 Vne[3]
U−B color index −0.08[2]
B−V color index −0.05[2]
Astrometry
Radial velocity (Rv)−6.6±2.9[4] km/s
Proper motion (μ) RA: −96.50[1] mas/yr
Dec.: −49.86[1] mas/yr
Parallax (π)18.12 ± 0.47 mas[1]
Distance180 ± 5 ly
(55 ± 1 pc)
Details
Mass2.89±0.03[5] M☉
Radius2.3[6] R☉
Luminosity151[3] L☉
Surface gravity (log g)3.99±0.14[7] cgs
Temperature11,305±384[7] K
Rotational velocity (v sin i)191±16[5] km/s
Age121[7] Myr
Other designations
κ1 Lup, CD−48° 9704, FK5 1398, HD 134481, HIP 74376, HR 5646, SAO 225525.[8]
Database references
SIMBADdata

Kappa1 Lupi is a solitary[9] star in the southern constellation of Lupus. It is visible to the naked eye with an apparent visual magnitude of 3.86,[2] and forms a double star with Kappa2 Lupi.[10] Based upon an annual parallax shift of 18.12[1] mas as seen from Earth, it is located about 180 light years from the Sun. Both Kappa1 Lupi and its neighbor Kappa2 Lupi are members of the Hyades Stream, which is a moving group that is coincident with the proper motions of the Hyades cluster.[11]

This is a B-type main sequence star with a stellar classification of B9.5 Vne.[3] The 'n' suffix indicates the spectrum shows "nebulous" absorption lines due to rapid rotation, while the 'e' means this is a Be star that displays Balmer series emission lines. With an estimated age of 195[3] million years, it is about 75% of the way through its life span on the main sequence.[5] The star is rotating with a projected rotational velocity of 191 km/s.[5] This rate of spin is giving the star an oblate shape with an equatorial bulge that is an estimated 9% larger than the polar radius.[12]

In Chinese astronomy, Kappa1 Lupi is called 騎陣將軍, Pinyin: Qízhènjiāngjūn, meaning Chariots and Cavalry General, because this star is marking itself and stand alone in Chariots and Cavalry General asterism, Root mansion (see : Chinese constellation).[13]

References

  1. ^ a b c d e f 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, S2CID 18759600.
  2. ^ a b c d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.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. ^ a b c d Levenhagen, R. S.; Leister, N. V. (2006), "Spectroscopic analysis of southern B and Be stars", Monthly Notices of the Royal Astronomical Society, 371 (1): 252–262, arXiv:astro-ph/0606149, Bibcode:2006MNRAS.371..252L, doi:10.1111/j.1365-2966.2006.10655.x, S2CID 16492030.
  4. ^ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
  5. ^ a b c d Zorec, J.; Royer, F. (January 2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  6. ^ Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics (3rd ed.), 367: 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
  7. ^ a b c David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
  8. ^ "kap Lup". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-03-07.((cite web)): CS1 maint: postscript (link)
  9. ^ Chini, R.; et al. (2012), "A spectroscopic survey on the multiplicity of high-mass stars", Monthly Notices of the Royal Astronomical Society, 424 (3): 1925, arXiv:1205.5238, Bibcode:2012MNRAS.424.1925C, doi:10.1111/j.1365-2966.2012.21317.x, S2CID 119120749.
  10. ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  11. ^ Eggen, Olin J. (1996), "The Stellar Content of Star Stream I", Astronomical Journal, 111: 1615, Bibcode:1996AJ....111.1615E, doi:10.1086/117901
  12. ^ Belle, G. T. (2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2, S2CID 119273474.
  13. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 6 月 29 日

External links

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