Kappa Coronae Borealis

Star in the constellation Corona Borealis From Wikipedia, the free encyclopedia

Kappa Coronae Borealis, Latinized from κ Coronae Borealis, is a star 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 evolved K-type star of spectral type K1IV, meaning it has completely exhausted its hydrogen supply at 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]

Quick facts Observation data Epoch J2000.0 Equinox J2000.0, Constellation ...
κ Coronae Borealis
Location of κ Coronae Borealis (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Corona Borealis[1]
Right ascension 15h 51m 13.9313s[2]
Declination +35° 39′ 26.574″[2]
Apparent magnitude (V) +4.79[3]
Characteristics
Evolutionary stage red giant branch[4][2]
Spectral type K0 III-IV[3]
Astrometry
Proper motion (μ) RA: âˆ’8.669[2] mas/yr
Dec.: âˆ’348.350[2] mas/yr
Parallax (π)33.3433±0.0800 mas[2]
Distance97.8 ± 0.2 ly
(29.99 ± 0.07 pc)
Absolute magnitude (MV)+2.37[1]
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
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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.[3]

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]

More information Companion (in order from star), Mass ...
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 — —
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See also

References

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