View source for Kepler-34b

{{Short description|Small circumbinary gas giant orbiting the Kepler-34 star system}}
{{Infobox planet
| name                     = Kepler-34b
<!-- DISCOVERY           -->
| discovered               = 01-11-2012
| discovery_method         = [[Methods_of_detecting_extrasolar_planets#Transit photometry|Transit]] ([[Kepler Mission]])
<!-- DESIGNATIONS        -->
<!-- ORBITAL             --> 
| epoch                    = BJD 2454969.2000
| apsis                    = astron
| semimajor                = {{convert|1.0896|±|0.0009|AU|km|abbr=on}}
| eccentricity             = 0.182 {{±|0.0016|0.0020}}
| period                   = 288.822 {{±|0.063|0.081}} [[day|d]]
| inclination              = 90.355 {{±|0.026|0.018}}
| asc_node                 = −1.74 {{±|0.14|0.16}}
| long_periastron          = 106.5 {{±|2.5|2.0}}
| star                     = [[Kepler-34]]
<!-- PHYS CHARS          --> 
| mean_radius              = 0.764 {{±|0.0012|0.0014}} {{Jupiter radius|link=y}}<br>8.56 {{Earth radius|link=y}}
| mass                     = 0.220 {{±|0.011|0.010}} {{Jupiter mass|link=y}}<br>(69.9 {{Earth mass|link=y}})
| density                  = 0.613 {{±|0.045|0.041}} [[gram|g]] [[cubic centimetre|cm<sup>−3</sup>]]
| surface_grav             = 936 {{±|57|54}} [[Metre per second squared|m/s²]] 
| single_temperature       = 323
<!-- ATMOSPHERE          --> 
<!-- NOTES               --> 
}}
'''Kepler-34b''' (formally '''Kepler-34(AB)b''') is a [[circumbinary planet]] announced with [[Kepler-35b]]. It is a small [[gas giant]] that orbits every ~288 days around two stars. Despite the planet's relatively long orbital period, its existence could be confirmed quickly due to transiting both of its host stars.

Kepler-34b was unlikely to form at its current orbit, and likely migrated early from its birth orbit beyond 1.5 [[astronomical unit|AU]] away from its parent binary stars, suffering multiple giant impacts in the process.<ref>{{citation|arxiv=1402.0509|title=Forming Circumbinary Planets: N -Body Simulations of Kepler-34|year=2014|doi=10.1088/2041-8205/782/1/L11 |last1=Lines |first1=S. |last2=Leinhardt |first2=Z. M. |last3=Paardekooper |first3=S. |last4=Baruteau |first4=C. |last5=Thebault |first5=P. |journal=The Astrophysical Journal |volume=782 |issue=1 |pages=L11 |bibcode=2014ApJ...782L..11L |s2cid=119214559 }}</ref> The eccentricity of its planetary orbit might have been acquired on the last stage of migration, due to interaction with the residual debris disk,<ref>{{citation|arxiv=1307.0713|title=Migration and gas accretion scenarios for the Kepler 16, 34, and 35 circumbinary planets|year=2013|doi=10.1051/0004-6361/201321777 |last1=Pierens |first1=A. |last2=Nelson |first2=R. P. |journal=Astronomy & Astrophysics |volume=556 |pages=A134 |bibcode=2013A&A...556A.134P |s2cid=118597351 }}</ref> or by ejection of a second planet.<ref>{{citation |last1=Gong |first1=Yan-Xiang |title=The Scattering Outcomes of ''Kepler'' Circumbinary Planets: Planet Mass Ratio |journal=The Astronomical Journal |volume=154 |issue=5 |page=179 |year=2017 |arxiv=1709.04433 |doi=10.3847/1538-3881/aa8c7c |s2cid=119085156 |last2=Ji |first2=Jianghui |bibcode=2017AJ....154..179G |doi-access=free }}</ref>

==References==
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{{Stars of Cygnus}}
{{2012 in space}}

[[Category:Exoplanets discovered in 2011]]
[[Category:Exoplanets discovered by the Kepler space telescope|34b]]
[[Category:Transiting exoplanets]]
[[Category:Circumbinary planets]]

{{Extrasolar-planet-stub}}
[[Category:Cygnus (constellation)]]