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Kepler-56

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Kepler-56[1][2][3]

Graphical sketch of the Kepler-56 system. The line of sight from Earth is illustrated by the dashed line, and dotted lines show the orbits of three detected companions in the system. The solid arrow marks the rotation axis of the host star, and the thin solid line marks the host star equator.
Credit:NASA GSFC/Ames/D Huber
Observation data
EpochJ2000.0[1]EquinoxJ2000.0[1]
Constellation Cygnus
Right ascension 19h35m02.0012s[4]
Declination +41° 52′ 18.692″[4]
Apparent magnitude(V) 13
Characteristics
Evolutionary stage red giant[5]
Spectral type K3III
Astrometry
Radial velocity(Rv)-53.740601[1]km/s
Proper motion(μ)RA:−6.596(12)mas/yr[4]
Dec.:−12.081(13)mas/yr[4]
Parallax(π)1.0755 ± 0.0118mas[4]
Distance3,030 ± 30ly
(930 ± 10pc)
Details[5]
Mass1.286±0.011M☉
Radius4.179±0.132R☉
Luminosity (bolometric)9.589±0.129L☉
Temperature4973±14K
Metallicity[Fe/H]0.0251±0.013dex
Age3.917±0.157Gyr
Other designations
Kepler-56,KOI-1241,KIC6448890,2MASS19350200+4152187
Database references
SIMBADdata

Kepler-56is ared giant[6]in constellationCygnusroughly 3,030 light-years (930 pc) away[4]with slightly more mass than theSun.

Characteristics

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Kepler-56 is a red giant star. This means it is no longer fusing hydrogen in its core and is off the main sequence. Its mass is around 1.3M⊙.Its radius is about 4.2R⊙,putting the star's density at about 0.025g/cm3.For reference, the Sun's density is about 1.408g/cm3.Its metallicity is about 0.0251Z0/X0.Its luminosity is about 9.6L⊙,and its effective temperature is 4,973 K (4,700 °C; 8,492 °F), classifying Kepler-56 as spectral class K3III.[5]

Kepler-56 is about 3.9 billion years old,[5]placing it as about 600 million years younger than our Sun. Its apparent magnitude is +13, making it too dim to be visible to the naked eye.

Planetary system

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In 2012, scientists discovered a two-planet planetary system around Kepler-56 via the transit method. Asteroseismological studies revealed that the orbits ofKepler-56bandKepler-56care coplanar but about 45° misaligned to the host star's equator. In addition, follow-up radial velocity measurements showed evidence of a gravitational perturbator.[6]It was confirmed in 2016 the perturbations are caused by third, non-transiting planet: Kepler-56d.[7]

The planetary system is very compact but is dynamically stable.[8]

Kepler-56 is expanding. As a result, it will devour Kepler-56b and Kepler-56c in 130 and 155 million years, respectively.[9][10]56d will be far enough to survive its parent star's red giant phase.

The Kepler-56 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b[2][11] 0.07MJ 0.1028 10.5034294 — 79.640° 3.606495320R🜨
c[3][12] 0.569MJ 0.1652 21.4050484 — 81.930° 7.844702558R🜨
d[7] >5.61±0.38MJ 2.16±0.08 1002±5 0.20±0.01 — —

References

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  1. ^abc"Kepler-56".SIMBAD.Centre de données astronomiques de Strasbourg.
  2. ^ab"Planet Kepler-56 b".Extrasolar Planets Encyclopaedia.Retrieved2013-10-18.
  3. ^ab"Planet Kepler-56 c".Extrasolar Planets Encyclopaedia.2018.
  4. ^abcdeVallenari, A.; et al. (Gaia collaboration) (2023)."GaiaData 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.S2CID244398875. Gaia DR3 record for this sourceatVizieR.
  5. ^abcdFellay, L.; Buldgen, G.; et al. (October 22, 2021)."Asteroseismology of evolved stars to constrain the internal transport of angular momentum".Astronomy & Astrophysics.654.12.arXiv:2108.02670.doi:10.1051/0004-6361/202140518.S2CID239652877.RetrievedMarch 30,2022.
  6. ^abHuber, Daniel; Carter, Joshua; et al. (October 21, 2013)."Stellar Spin-Orbit Misalignment in a Multiplanet System".Science.342(6156): 331–334.arXiv:1310.4503.Bibcode:2013Sci...342..331H.doi:10.1126/science.1242066.PMID24136961.S2CID1056370.
  7. ^abOtor, Oderah Justin; Montet, Benjamin T.; et al. (22 September 2016)."The Orbit and Mass of the Third Planet in the Kepler-56 System".The Astronomical Journal.152(6). Cornell University: 165.arXiv:1608.03627v2.Bibcode:2016AJ....152..165O.doi:10.3847/0004-6256/152/6/165.ISSN0004-6256.
  8. ^Denham, Paul; Naoz, Smadar; et al. (29 October 2018)."Hidden planetary friends: on the stability of two-planet systems in the presence of a distant, inclined companion".Monthly Notices of the Royal Astronomical Society.482(3): 4146–4154.arXiv:1802.00447.doi:10.1093/mnras/sty2830.ISSN0035-8711.
  9. ^Kramer, Miriam (June 10, 2014)."Chow Down! Star Will Devour 2 Alien Planets".Space.Retrieved24 February2022.
  10. ^Li, Gongjie;Naoz, Smadar;et al. (October 1, 2014)."The Dynamics of the Multi-planet System Orbiting Kepler-56".The Astrophysical Journal.794(2): 131.arXiv:1407.2249.Bibcode:2014ApJ...794..131L.doi:10.1088/0004-637X/794/2/131.S2CID56224888.
  11. ^"KOI-1241.02 -- Extra-solar Confirmed Planet".SIMBAD.
  12. ^"KOI-1241.01 -- Extra-solar Confirmed Planet".SIMBAD.
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