Astronomy:Kappa Coronae Borealis

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Short description: Star in the constellation Corona Borealis
κ Coronae Borealis
Corona Borealis constellation map.svg
Red circle.svg
Location of κ Coronae Borealis (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Corona Borealis
Right ascension  15h 51m 13.9315s[1]
Declination +35° 39′ 26.5647″[1]
Apparent magnitude (V) +4.79[2]
Characteristics
Spectral type K0 III-IV[2]
Astrometry
Proper motion (μ) RA: −8.792±0.177[1] mas/yr
Dec.: −347.766±0.202[1] mas/yr
Parallax (π)33.2328 ± 0.1083[1] mas
Distance98.1 ± 0.3 ly
(30.09 ± 0.10 pc)
Absolute magnitude (MV)+2.37[3]
Details[4]
Mass1.32±0.10 M☉
Radius4.77±0.07 R☉
Luminosity11.6±0.3 L☉
Surface gravity (log g)3.15±0.14 cgs
Temperature4,870±47 K
Metallicity [Fe/H]+0.13±0.03 dex
Other designations
κ CrB, 11 CrB, HD 142091, HIP 77655, HR 5901, SAO 64948[5]
Database references
SIMBADdata

Kappa Coronae Borealis, Latinized from κ Coronae Borealis, is a star approximately 98 light years away in the constellation of Corona Borealis. The apparent magnitude is +4.82 (4.17 trillion times fainter than the Sun) and the absolute magnitude is +2.35 (9.82 times brighter than the Sun). It is an orange K-type subgiant star of spectral type K1IV, meaning it has almost completely exhausted its hydrogen supply in its core. It is 1.32 times as massive as the Sun yet has brightened to 11.6 times its luminosity. Around 2.5 billion years old, it was formerly an A-type main sequence star.[6]

Dust disk

In March 2013, it was announced that resolved images of at least one dust disk surrounding Kappa Coronae Borealis were captured, making it the first subgiant to host such circumstellar belt.[6] The disk extends out from 50 AU to 180 AU, and there is an estimated 0.016 M⊕ of dust.[7]

Planetary system

In October 2007, a giant planet was found by Johnson et al., who used the radial velocity method.[8] In 2012 it was confirmed.[2]

This planet was assumed to be outside the habitable zone on the assumption that the star is K1IVa.[9] Given the star's luminosity, the planet is more likely on the zone's inner edge.[10]

The width of the circumstellar belt suggests the presence of a second planetary companion of the star, either within it or between two narrower belts.[6]

The Kappa Coronae Borealis planetary system[11]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥1.811±0.057 MJ 2.65±0.13 1285±14 0.167±0.032 — —

See also

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 Sato, Bun'ei et al. (2012). "Substellar Companions to Seven Evolved Intermediate-Mass Stars". Publications of the Astronomical Society of Japan 64 (6): 135. doi:10.1093/pasj/64.6.135. Bibcode: 2012PASJ...64..135S. https://academic.oup.com/pasj/article/64/6/135/1422181. 
  3. ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  4. ↑ White, T. R. et al. (July 2018). "Interferometric diameters of five evolved intermediate-mass planet-hosting stars measured with PAVO at the CHARA Array". Monthly Notices of the Royal Astronomical Society 477 (4): 4403–4413. doi:10.1093/mnras/sty898. Bibcode: 2018MNRAS.477.4403W. 
  5. ↑ "Kappa Coronae Borealis". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Kappa+Coronae+Borealis. 
  6. ↑ 6.0 6.1 6.2 Bonsor, Amy (2013). "Spatially resolved images of dust belt(s) around the planet-hosting subgiant κ CrB". MNRAS 431 (4): 3025–3035. doi:10.1093/mnras/stt367. Bibcode: 2013MNRAS.431.3025B. 
  7. ↑ Lovell, J. B.; Wyatt, M. C.; Kalas, P.; Kennedy, G. M.; Marino, S.; Bonsor, A.; Penoyre, Z.; Fulton, B. J. et al. (2022). "High-resolution ALMA and HST imaging of κ CrB: A broad debris disc around a post-main-sequence star with low-mass companions". Monthly Notices of the Royal Astronomical Society 517 (2): 2546–2566. doi:10.1093/mnras/stac2782. Bibcode: 2022MNRAS.517.2546L. 
  8. ↑ Johnson, John Asher et al. (2008). "Retired A Stars and Their Companions. II. Jovian Planets Orbiting κ CrB and HD 167042". The Astrophysical Journal 675 (1): 784–789. doi:10.1086/526453. Bibcode: 2008ApJ...675..784J. 
  9. ↑ "Planet kappa CrB b". http://exoplanet.hanno-rein.de/system.php?id=kappa+CrB+b. 
  10. ↑ An earth-analogue should be slightly more than 3 AU away: square root of luminosity 12.9.
  11. ↑ Luhn, Jacob K. et al. (2019). "Retired A Stars and Their Companions. VIII. 15 New Planetary Signals around Subgiants and Transit Parameters for California Planet Search Planets with Subgiant Hosts". The Astronomical Journal 157 (4): 149. doi:10.3847/1538-3881/aaf5d0. Bibcode: 2019AJ....157..149L. 

Coordinates: Sky map 15h 51m 13.9315s, +35° 39′ 26.575″



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