Kepler-56b

Kepler-56b
Exoplanet List of exoplanets

A diagram of the planetary system of Kepler-56
Parent star
Star Kepler-56
Constellation Cygnus
Right ascension (α) 19h 35m 02.0014s[1]
Declination (δ) +41° 52′ 18.692″[1]
Apparent magnitude (mV) 13.0[2]
Distance3060±80[1] ly
(940±20[1] pc)
Mass (m) 1.29+0.03
−0.04[3] M☉
Radius (r) 4.19+0.21
−0.19[3] R☉
Temperature (T) 4911+34
−58[3] K
Metallicity [Fe/H] −0.03 ± 0.02[3]
Age 4.4 Gyr[3] Gyr
Orbital elements
Semi-major axis(a) 0.1028 ± 0.0037[4] AU
Orbital period(P) 10.5016+0.0011
−0.0010[4] d
Time of transit (Tt) 2454978.2556+0.0056
−0.0057[4] JD
Physical characteristics
Mass(m)22.1+3.9
−3.6[4] M⊕
Radius(r)6.51+0.29
−0.28[4] R⊕
Density(ρ)0.442+0.080
−0.072[4] g cm−3
Discovery information
Discovery date 16 October 2013
Discoverer(s) Daniel Huber et al.[4]
Discovery method Transit method
Other detection methods Transit-timing variation
Discovery status Confirmed
Database references
Extrasolar Planets
Encyclopaedia		data
SIMBADdata
Exoplanet Archivedata
Open Exoplanet Cataloguedata

Kepler-56b (KOI-1241.02)[5] is an exoplanet located roughly 3,060 light years away. It is somewhat larger than Neptune[6] and orbits its parent star Kepler-56 and was discovered in 2012 by the Kepler Space Telescope.

Planetary orbit

Kepler-56b is about 0.1028 AU away from its host star[4] (about one-tenth of the distance between Earth to the Sun), making it even closer to its parent star than Mercury and Venus. It takes 10.5 days for Kepler-56b to complete a full orbit around Kepler-56.[4] Further research shows that Kepler-56b's orbit is about 45° misaligned to the host star's equator. Later radial velocity measurements have revealed evidence of a gravitational perturbation but currently it is not clear if it is a nearby star or a third planet (a possible Kepler-56d).

Both Kepler-56b and Kepler-56c will be devoured by their parent star in about 130 and 155 million years.[7] Even further research shows that it will have its atmosphere boiled away by intense heat from the star, and it will be stretched by the strengthening stellar tides.[7] The measured mass of Kepler-56b is about 30% as large as Neptune's mass, but its radius is roughly 70% as large as Neptune's. Therefore, Kepler-56b should have a hydrogen/helium envelope containing a significant fraction of its total mass.[8][9] Similarly to Kepler-11b and Kepler-11c, the envelope's light elements are susceptible to photo-evaporation caused by radiation from the central star. For example, it has been calculated that Kepler-11c lost over 50% of its hydrogen/helium envelope after formation.[10] However, the larger mass of Kepler-56b, compared to that of Kepler-11c, reduces the efficiency of mass loss.[10] Nonetheless, the planet may have been significantly more massive in the past and may keep losing mass in the future.

References

  1. 1 2 3 4 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. ↑ "Kepler-56 b". The Extrasolar Planet Encyclopaedia. exoplanet.eu. Retrieved 2016-01-02.
  3. 1 2 3 4 5 Morton, Timothy D.; et al. (2016). "False positive probabilities for all Kepler Objects of Interest: 1284 newly validated planets and 428 likely false positives". The Astrophysical Journal. 822 (2): 86. arXiv:1605.02825. Bibcode:2016ApJ...822...86M. doi:10.3847/0004-637X/822/2/86.
  4. 1 2 3 4 5 6 7 8 9 Huber, D.; et al. (2013). "Stellar Spin-Orbit Misalignment in a Multiplanet System". Science. 342 (6156): 331. arXiv:1310.4503. Bibcode:2013Sci...342..331H. doi:10.1126/science.1242066. PMID 24136961.
  5. ↑ "KOI-1241.02". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-07.
  6. ↑ "NASA Exoplanet Archive". NASA Exoplanet Archive. Operated by the California Institute of Technology, under contract with NASA.
  7. 1 2 Charles Poladian (2014-06-03). "Cosmic Snack: Planets Kepler-56b And Kepler-56c Will Be Swallowed Whole By Host Star". International Business Times. Retrieved 2017-09-07.
  8. ↑ Lissauer, J. J.; Hubickyj, O.; D'Angelo, G.; Bodenheimer, P. (2009). "Models of Jupiter's growth incorporating thermal and hydrodynamic constraints". Icarus. 199 (2): 338–350. arXiv:0810.5186. Bibcode:2009Icar..199..338L. doi:10.1016/j.icarus.2008.10.004.
  9. ↑ D'Angelo, G.; Weidenschilling, S. J.; Lissauer, J. J.; Bodenheimer, P. (2014). "Growth of Jupiter: Enhancement of core accretion by a voluminous low-mass envelope". Icarus. 241: 298–312. arXiv:1405.7305. Bibcode:2014Icar..241..298D. doi:10.1016/j.icarus.2014.06.029.
  10. 1 2 D'Angelo, G.; Bodenheimer, P. (2016). "In Situ and Ex Situ Formation Models of Kepler 11 Planets". The Astrophysical Journal. 828 (1): id. 33. arXiv:1606.08088. Bibcode:2016ApJ...828...33D. doi:10.3847/0004-637X/828/1/33.

Further reading

  • Steffen, Jason H; Fabrycky, Daniel C; Agol, Eric; et al. (20 August 2012). "Transit Timing Observations from Kepler: VII. Confirmation of 27 planets in 13 multiplanet systems via Transit Timing Variations and orbital stability". Mon. Not. R. Astron. Soc. 428 (2): 1077. arXiv:1208.3499. Bibcode:2013MNRAS.428.1077S. doi:10.1093/mnras/sts090.
  • "Kepler-56b". kepler.nasa.gov. Retrieved 2016-01-02.
  • Megan Smith (8 June 2014). "Star to Swallow not One, but Two Exoplanets". Futurism LLC.


This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.