Kappa Ophiuchi
Location of κ Ophiuchi (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Ophiuchus
Right ascension 16h 57m 40.09785s[1]
Declination +09° 22′ 30.1126″[1]
Apparent magnitude (V) 3.20[2]
Characteristics
Spectral type K2 III[3]
U−B color index +1.16[2]
B−V color index +1.16[2]
Astrometry
Radial velocity (Rv)−55.85±0.10[4] km/s
Proper motion (μ) RA: –292.13[1] mas/yr
Dec.: –10.38[1] mas/yr
Parallax (π)35.66 ± 0.20 mas[1]
Distance91.5 ± 0.5 ly
(28.0 ± 0.2 pc)
Absolute magnitude (MV)+0.964
Details
Mass1.19±0.14[5] M☉
Radius11[4] R☉
Luminosity46[4] L☉
Surface gravity (log g)2.5[4] cgs
Temperature4,529[4] K
Metallicity [Fe/H]–0.03[4] dex
Rotational velocity (v sin i)4.7[4] km/s
Other designations
κ Oph, 27 Ophiuchi, BD+09 3298, HD 153210, HIP 83000, HR 6299, SAO 121962[6]
Database references
SIMBADdata

Kappa Ophiuchi, Latinized from κ Ophiuchi, is a star in the equatorial constellation Ophiuchus. It is a suspected variable star with an average apparent visual magnitude of 3.20,[2] making it visible to the naked eye and one of the brighter members of this constellation. Based upon parallax measurements made during the Hipparcos mission, it is situated at a distance of around 91.5 light-years (28.1 parsecs) from Earth.[1] The overall brightness of the star is diminished by 0.11 magnitudes due to extinction from intervening matter along the line of sight.[7]

The spectrum of this star matches a stellar classification of K2 III,[3] with the luminosity class of 'III' indicating this is a giant star that has exhausted the hydrogen at its core and evolved away from the main sequence of stars like the Sun. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified.[8] It is 19% more massive than the Sun, but the outer envelope has expanded to around 11 times the Sun's radius.[4] With its enlarged size, it is radiating 46 times the luminosity of the Sun[4] from its outer atmosphere at an effective temperature of 4,529 K.[4] This is cooler than the Sun's surface and gives Kappa Ophiuchi the orange-hued glow of a K-type star.[9]

Although designated as a variable star,[6] observations with the Hipparcos satellite showed a variation of no more than 0.02 in magnitude. In designating this as a suspected variable star, it is possible that Kappa Ophiuchi was mistaken for Chi Ophiuchi, which is a variable star.[10] Kappa Ophiuchi belongs to an evolutionary branch known as the red clump, making it a clump giant.[11] The surface abundance of elements other than hydrogen and helium, what astronomers term the star's metallicity, is similar to the abundances of those elements in the Sun.[4]

References

  1. ^ a b c d e f van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752v1, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600 Note: see VizieR catalogue I/311.
  2. ^ a b c d Jennens, P. A.; Helfer, H. L. (September 1975), "A new photometric metal abundance and luminosity calibration for field G and K giants.", Monthly Notices of the Royal Astronomical Society, 172 (3): 667–679, Bibcode:1975MNRAS.172..667J, doi:10.1093/mnras/172.3.667
  3. ^ a b Morgan, W. W.; Keenan, P. C. (1973), "Spectral Classification", Annual Review of Astronomy and Astrophysics, 11: 29–50, Bibcode:1973ARA&A..11...29M, doi:10.1146/annurev.aa.11.090173.000333
  4. ^ a b c d e f g h i j k Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209
  5. ^ Stello, D.; et al. (2008), "Oscillating K giants with the WIRE Satellite: Determination of their asteroseismic masses", The Astrophysical Journal Letters, 674 (1): L53–L56, arXiv:0801.2155, Bibcode:2008ApJ...674L..53S, doi:10.1086/528936, S2CID 15094067
  6. ^ a b "kap Oph". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-02-03.
  7. ^ Famaey, B.; et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics, 430: 165–186, arXiv:astro-ph/0409579, Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272, S2CID 17804304
  8. ^ Garrison, R. F. (December 1993), "Anchor Points for the MK System of Spectral Classification", Bulletin of the American Astronomical Society, 25: 1319, Bibcode:1993AAS...183.1710G, archived from the original on 2019-06-25, retrieved 2012-02-04
  9. ^ "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 2012-01-16
  10. ^ Kaler, James B., "Kappa Ophiuchi", Stars, University of Illinois, retrieved 2012-03-12
  11. ^ Adelman, Saul J. (2001), "On the Photometric Variability of Red Clump Giants", Baltic Astronomy, 10 (4): 593–597, Bibcode:2001BaltA..10..593A, doi:10.1515/astro-2001-0404
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