Kepler-47

Kepler-47
Observation data
Epoch J2000      Equinox J2000
Constellation Cygnus
Right ascension 19h 41m 11.4985s[1]
Declination +46° 55′ 13.705″[1]
Apparent magnitude (V) 15.8
Characteristics
Evolutionary stage Main sequence
Spectral type G6V / M4V
Astrometry
Proper motion (μ) RA: −3.494±0.057[1] mas/yr
Dec.: −10.065±0.055[1] mas/yr
Parallax (π)0.9476 ± 0.0289[1] mas
Distance3,400 ± 100 ly
(1,060 ± 30 pc)
Orbit
PrimaryKepler-47A
CompanionKepler-47B
Period (P)7.45 days
Semi-major axis (a)0.0836 AU
Details[2][3]
Kepler-47A
Mass1.043 ± 0.055[2] M☉
Radius0.964 ± 0.017[2] R☉
Luminosity0.84[2] L☉
Surface gravity (log g)4.42 ± 0.1 cgs
Temperature5636 ± 100[2] K
Metallicity [Fe/H]−0.25 ± 0.08[2] dex
Rotational velocity (v sin i)4.1+0.5
−0.35 km/s
Age4–5 Gyr
Kepler-47B
Mass0.362 ± 0.013[2] M☉
Radius0.3506 ± 0.006[2] R☉
Luminosity0.01[2] L☉
Temperature3357 ± 100[2] K
Age4–5 Gyr
Other designations
2MASS J19411149+4655136, KOI-3154, KIC 10020423
Database references
SIMBADdata
KICdata

Kepler-47 is a binary star system with at least three planets in orbit around the pair of stars located about 3,400 light-years away from Earth.[1][4][2] The first two planets announced are designated Kepler-47b, and Kepler-47c. Kepler-47 is the first circumbinary multi-planet system discovered by the Kepler mission.[3] The outermost of the planets is a gas giant orbiting within the habitable zone of the stars.[5] Because most stars are binary,[6] the discovery that multi-planet systems can form in such a system impacts theories of planetary formation.

A group of scientists from NASA and Tel-Aviv University in Israel discovered the system via NASA's Kepler space observatory in 2012.[7] In November 2013, confirmation of a third planet, Kepler-47d was announced,[8] with a shorter orbit than c.

Nomenclature and history

The Kepler Space Telescope search volume, in the context of the Milky Way Galaxy.

Prior to Kepler observation, Kepler-47 had the 2MASS catalogue number 2MASS J19411149+4655136. In the Kepler Input Catalog it has the designation of KIC 10020423, and when it was found to have transiting planet candidates it was given the Kepler object of interest number of KOI-3154.

Planetary candidates were detected around the star by NASA's Kepler Mission, a mission tasked with discovering planets in transit around their stars. The transit method that Kepler uses involves detecting dips in brightness in stars. These dips in brightness can be interpreted as planets whose orbits pass in front of their stars from the perspective of Earth, although other phenomenon can also be responsible which is why the term planetary candidate is used.[9]

Following the acceptance of the discovery paper, the Kepler team provided an additional moniker for the system of "Kepler-47".[10] The discoverers referred to the star as Kepler-47, which is the normal procedure for naming the exoplanets discovered by the spacecraft.[2] Hence, this is the name used by the public to refer to the star and its planet.

Candidate planets that are associated with stars studied by the Kepler Mission are assigned the designations ".01", ".02", ".03" etc. after the star's name, in the order of discovery.[11] If planet candidates are detected simultaneously, then the ordering follows the order of orbital periods from shortest to longest.[11] Following these rules, there was two candidate planets detected, with orbital periods of 49.51 and 303.158 days.

The designation b, c and d derive from the order of discovery. The designation of b is given to the first planet orbiting a given star, and d to the farthest.[12] In the case of Kepler-47, there was initially two detected, so the letters b and c are used. When a third planet was confirmed, it was given the letter d.

Stellar characteristics

Kepler-47 is a binary star system composed of a G-type main sequence star (Kepler-47A) and a red dwarf star (Kepler-47B). The stars orbit each other about every 7.45 days. The stars have 104% and 35% of the Sun's mass, and 96% and 35% of the Sun's radius, respectively.[2] They have temperatures of 5636 K and 3357 K.[2] Based on the stellar characteristics and orbital dynamics, an estimated age of 4–5 billion years for the system is possible. In comparison, the Sun is about 4.6 billion years old[13] and has a temperature of 5778 K.[14]

The primary star is somewhat metal-poor, with a metallicity ([Fe/H]) of about –0.25, or about 56% of the amount of iron and other heavier metals found in the Sun.[2] Both of the stars' luminosities are typical for their kind, with a luminosities of around 84% and 1% of that of the solar luminosity, respectively.[2]

The apparent magnitude of the system, or how bright it appears from Earth's perspective, is about 15.8. Therefore, it is too dim to be seen with the naked eye.

Planetary system

The Kepler-47 planetary system[3]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 8.427 ± 0.62 M⊕ 0.2956 ± 0.0047 49.51 ± 0.04 <0.035 89.59 ± 0.5° 3.03 ± 0.12 R⊕
d (unconfirmed) — 0.5–0.7 187.3 ~0 ~89.8° 3.8–4.1 R⊕
c 23.17 ± 1.97 M⊕ 0.989 ± 0.016 303.158 ± 0.072 <0.411 89.825 ± 0.010° 4.61 ±  0.20 R⊕

The binary system is known to host three planets, all larger than Earth with no solid surface. The innermost planet, Kepler-47b, is a gas giant and resides close to its parent stars and therefore is inhospitable to life. It is thought to be smaller than Kepler-47c and is roughly three times the radius of Earth.[3] The second planet, Kepler-47c, is also a gas giant and the outermost planet. It is situated within the habitable zone and its radius is 4 times the Earth's. Although it is assumed Kepler-47c is not capable of harboring life,[15] it is marginally larger than Neptune and could possibly have a dense atmosphere of water vapor.[16] The latest exoplanet to be discovered in the system was Kepler-47d, announced as being discovered in November 2013. This planet is about the size of planet "c", but orbits farther in then c does. It completes an orbit every 187.3 days.[8]

See also

References

  1. 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 Data Release 2 Vizier catalog entry
  2. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 Orosz, Jerome A.; Welsh, William F.; Carter, Joshua A.; Fabrycky, Daniel C.; Cochran, William D.; Endl, Michael; Ford, Eric B.; Haghighipour, Nader; MacQueen, Phillip J.; Mazeh, Tsevi; Sanchis-Ojeda, Roberto; Short, Donald R.; Torres, Guillermo; Agol, Eric; Buchhave, Lars A.; Doyle, Laurance R.; Isaacson, Howard; Lissauer, Jack J.; Marcy, Geoffrey W.; Shporer, Avi; Windmiller, Gur; Barclay, Thomas; Boss, Alan P.; Clarke, Bruce D.; Fortney, Jonathan; Geary, John C.; Holman, Matthew J.; Huber, Daniel; Jenkins, Jon M.; et al. (2012). "Kepler-47: A Transiting Circumbinary Multi-Planet System". Science. 337 (6101): 1511–4. arXiv:1208.5489. Bibcode:2012Sci...337.1511O. doi:10.1126/science.1228380. PMID 22933522.
  3. 1 2 3 4 "NASA's Kepler Discovers Multiple Planets Orbiting a Pair of Stars". NASA. 2012-08-28. Retrieved 2 September 2012. Kepler mission has discovered multiple transiting planets orbiting two suns for the first time
  4. ↑ "BBC News - Tatooine-like double-star systems can host planets". Bbc.co.uk. 2012-08-29. Retrieved 2012-11-04.
  5. ↑ "NASA's Kepler discovers multiple planets orbiting a pair of stars". Sciencedaily.com. 2012-08-28. arXiv:1208.5489. Bibcode:2012Sci...337.1511O. doi:10.1126/science.1228380. Retrieved 2012-11-04.
  6. ↑ Quintana, Elisa, V.; et al. (November 2006), "Terrestrial planet formation surrounding close binary stars", Icarus, 185 (1): 1–20, arXiv:astro-ph/0607222, Bibcode:2006Icar..185....1Q, doi:10.1016/j.icarus.2006.06.016
  7. ↑ Shamah, David (30 August 2012). "New worlds discovered, courtesy of US-Israel team". The Times of Israel. Retrieved 30 August 2012.
  8. 1 2 http://nexsci.caltech.edu/conferences/KeplerII/abstracts_talks/Orosz.pdf
  9. ↑ Morton, Timothy; Johnson, John (23 August 2011). "On the Low False Positive Probabilities of Kepler Planet Candidates". The Astrophysical Journal. 738 (2): 170. arXiv:1101.5630. Bibcode:2011ApJ...738..170M. doi:10.1088/0004-637X/738/2/170. Retrieved 2 March 2014.
  10. ↑ NASA (27 January 2014). "Kepler – Discoveries – Summary Table". NASA. Retrieved 1 March 2014.
  11. 1 2 "Kepler Input Catalog search result". Space Telescope Science Institute. Retrieved 25 July 2015.
  12. ↑ Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707 [astro-ph.SR].
  13. ↑ Fraser Cain (16 September 2008). "How Old is the Sun?". Universe Today. Retrieved 19 February 2011.
  14. ↑ Fraser Cain (September 15, 2008). "Temperature of the Sun". Universe Today. Retrieved 19 February 2011.
  15. ↑ "Tatooine-like double-star systems can host planets".
  16. ↑ "Two planets ... Two stars: Nasa detects strange new solar system (and one of the planets occupies the life-supporting 'Goldilocks zone')". Daily Mail. dailymail.co.uk. 30 August 2012.

Coordinates: 19h 41m 11.5s, +46° 55′ 12″

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