Kepler-34b

{{Short description|Small circumbinary gas giant orbiting the Kepler-34 star system}}

{{Infobox planet

| name = Kepler-34b

| discovered = 01-11-2012

| discovery_method = Transit (Kepler Mission)

| 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}} 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

| mean_radius = 0.764 {{±|0.0012|0.0014}} {{Jupiter radius|link=y}}
8.56 {{Earth radius|link=y}}

| mass = 0.220 {{±|0.011|0.010}} {{Jupiter mass|link=y}}
(69.9 {{Earth mass|link=y}})

| density = 0.613 {{±|0.045|0.041}} g cm⁻³

| surface_grav = 936 {{±|57|54}} m/s²

| single_temperature = 323

}}

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 AU away from its parent binary stars, suffering multiple giant impacts in the process.{{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 }} The eccentricity of its planetary orbit might have been acquired on the last stage of migration, due to interaction with the residual debris disk,{{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 }} or by ejection of a second planet.{{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 }}