Kepler-26

The Kepler-26 system, with the circumstellar habitable zone in green.
Observation data
Epoch J2000      Equinox J2000
Constellation Lyra[1]
Right ascension 18h 59m 45.8407s[2]
Declination +46° 33′ 59.438″[2]
Apparent magnitude (V) 15.473[3]
Characteristics
Spectral type M0V[4]
Astrometry
Proper motion (μ) RA: 9.540±0.053[2] mas/yr
Dec.: −13.961±0.055[2] mas/yr
Parallax (π)2.9537 ± 0.0270 mas[2]
Distance1,100 ± 10 ly
(339 ± 3 pc)
Details
Mass0.65[3] M☉
Radius0.59[3] R☉
Luminosity0.1[3] L☉
Temperature4500[3] K
Metallicity [Fe/H]-0.21[3] dex
Rotation17.918±0.005 days[5]
Rotational velocity (v sin i)1.9[3] km/s
Other designations
KOI-250, KIC 9757613, 2MASS J18594583+4633595, Gaia DR2 2107317358665730688
Database references
SIMBADdata
KICdata

Kepler-26 is a star in the northern constellation of Lyra. It is located at the celestial coordinates: Right Ascension 18h 59m 45.8407s Declination +46° 33′ 59.438″.[2] With an apparent visual magnitude of 15.5,[3] this star is too faint to be seen with the naked eye.

Planetary system

The two planets, Kepler-26b and Kepler-26c, were discovered by transit method in late 2011,[6] and classified as small (sub-Neptune) gas giants in 2016.[7] In 2012, the planetary candidate Kepler-26d was also detected, and confirmed in 2014.[8] The planet Kepler-26e was discovered on a much wider orbit in 2014.[9]

The Kepler-26 planetary system[4][7][10]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
d — 0.039 3.543919 — — 1.2 R🜨
b 5.1±0.7 M🜨 0.085 12.2829 — — 2.78±0.11 R🜨
c 6.2±0.7 M🜨 0.107 17.2513 — — 2.72±0.12 R🜨
e — 0.22 46.827915 — — 2.1 R🜨

References

  1. ↑ "Lyra – constellation boundary", The Constellations, International Astronomical Union, retrieved 2011-12-15
  2. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  3. 1 2 3 4 5 6 7 8 Kepler-26b, NASA Ames Research Center, archived from the original on 2012-05-03, retrieved 2011-12-06
  4. 1 2 Schneider, Jean, "Star: Kepler-26", Extrasolar Planets Encyclopaedia, archived from the original on 2012-05-05, retrieved 2013-12-18
  5. ↑ McQuillan, A.; Mazeh, T.; Aigrain, S. (2013). "Stellar Rotation Periods of The Kepler objects of Interest: A Dearth of Close-In Planets Around Fast Rotators". The Astrophysical Journal Letters. 775 (1). L11. arXiv:1308.1845. Bibcode:2013ApJ...775L..11M. doi:10.1088/2041-8205/775/1/L11. S2CID 118557681.
  6. ↑ Steffen, Jason H.; Fabrycky, Daniel C.; Ford, Eric B.; Carter, Joshua A.; Desert, Jean-Michel; Fressin, Francois; Holman, Matthew J.; Lissauer, Jack J.; Moorhead, Althea V.; Rowe, Jason F.; Ragozzine, Darin; Welsh, William F.; Batalha, Natalie M.; Borucki, William J.; Buchhave, Lars A.; Bryson, Steve; Caldwell, Douglas A.; Charbonneau, David; Ciardi, David R.; Cochran, William D.; Endl, Michael; Everett, Mark E.; Gautier III, Thomas N.; Gilliland, Ron L.; Girouard, Forrest R.; Jenkins, Jon M.; Horch, Elliott; Howell, Steve B.; Isaacson, Howard; et al. (2012), "Transit Timing Observations from Kepler: III. Confirmation of 4 Multiple Planet Systems by a Fourier-Domain Study of Anti-correlated Transit Timing Variations", Monthly Notices of the Royal Astronomical Society, 421 (3): 2342, arXiv:1201.5412, Bibcode:2012MNRAS.421.2342S, doi:10.1111/j.1365-2966.2012.20467.x, S2CID 11898578
  7. 1 2 Cubillos, Patricio; Erkaev, Nikolai V.; Juvan, Ines; Fossati, Luca; Johnstone, Colin P.; Lammer, Helmut; Lendl, Monika; Odert, Petra; Kislyakova, Kristina G. (2016), "An overabundance of low-density Neptune-like planets", Monthly Notices of the Royal Astronomical Society, 466 (2): 1868–1879, arXiv:1611.09236, doi:10.1093/mnras/stw3103, S2CID 119408956
  8. ↑ Rowe, Jason F.; Bryson, Stephen T.; Marcy, Geoffrey W.; Lissauer, Jack J.; Jontof-Hutter, Daniel; Mullally, Fergal; Gilliland, Ronald L.; Issacson, Howard; Ford, Eric; Howell, Steve B.; Borucki, William J.; Haas, Michael; Huber, Daniel; Steffen, Jason H.; Thompson, Susan E.; Quintana, Elisa; Barclay, Thomas; Still, Martin; Fortney, Jonathan; Gautier, T. N.; Hunter, Roger; Caldwell, Douglas A.; Ciardi, David R.; Devore, Edna; Cochran, William; Jenkins, Jon; Agol, Eric; Carter, Joshua A.; Geary, John (2014). "Validation Ofkepler's Multiple Planet Candidates. III. Light Curve Analysis and Announcement of Hundreds of New Multi-Planet Systems". The Astrophysical Journal. 784 (1): 45. arXiv:1402.6534. Bibcode:2014ApJ...784...45R. doi:10.1088/0004-637X/784/1/45. S2CID 119118620.
  9. ↑ Planet Kepler-26 e on exoplanet.eu
  10. ↑ Jontof-Hutter, Daniel; Ford, Eric B.; Rowe, Jason F.; Lissauer, Jack J.; Fabrycky, Daniel C.; Christa Van Laerhoven; Agol, Eric; Deck, Katherine M.; Holczer, Tomer; Mazeh, Tsevi (2015), Secure TTV Mass Measurements: Ten Kepler Exoplanets between 3 and 8 M🜨 with Diverse Densities and Incident Fluxes, arXiv:1512.02003, doi:10.3847/0004-637X/820/1/39, S2CID 11322397
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