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| epoch = J2000
| constell = [[Cygnus (constellation)|Cygnus]]
| ra = {{RA|19|51|22.17421744}}<ref name="Gaia DR2DR3"/>
| dec = {{DEC|+46|34|27.390391}}<ref name="Gaia DR2DR3"/>
| appmag_v = 16.0<ref name="EU">{{cite webencyclopedia|title=Notes on Kepler-32 b|url=httphttps://exoplanet.eu/catalog/keplerkepler_32_b-32_b-1069/|encyclopedia=[[Extrasolar Planets Encyclopaedia]]|access-date=21 January 2017}}</ref>
}}
{{Starbox character
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{{Starbox astrometry
| radial_v =
| prop_mo_ra = {{val|−13.618762|0.058(31)}}<ref name="Gaia DR2"/>
| prop_mo_dec = {{val|19.646586|0.068(32)}}
| pm_footnote = <ref name="Gaia DR2DR3"/>
| parallax = 3.05950960
| p_error = 0.03220276
| parallax_footnote = <ref name="Gaia DR2DR3"/>
| absmag_v =
}}
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}}
{{Starbox end}}
'''Kepler-32''' is an [[M-type star|M-type]] [[main sequence]] [[star]] located about 10701053 [[light years]] from Earth, in the [[Cygnus (constellation)|constellation of Cygnus]]. Discovered in January 2012 by the [[Kepler (spacecraft)|Kepler spacecraft]],<ref name=NBC>{{cite web|last=NBC|title=100 billion alien planets fill our galaxy: study|date=3 January 2013 |url=httphttps://www.nbcnews.com/id/50348563/ns/technology_and_science-space/#.US-dW4Z8wVBwbna50348563|publisher=[[NBC News]]|access-date=28 February 2013}}</ref> it shows a 0.58 ± 0.05 [[solar mass]] ({{Solar mass|link=yes}}), a 0.53 ± 0.04 [[solar radius]] ({{Solar radius|link=yes}}), and temperature of 3900.0 [[Kelvin|K]], making it half the mass and radius of the [[Sun]], two-thirds its temperature and 5% its luminosity.<ref name=Swift>{{Cite journal|last=Swift|first=Jonathan J.|title=Characterizing the Cool KOIs IV: Kepler-32 as a prototype for the formation of compact planetary systems throughout the Galaxy|journal=The Astrophysical Journal|volume=764|pages=105|year=2012|issue=1|arxiv=1301.0023|doi=10.1088/0004-637X/764/1/105|bibcode=2013ApJ...764..105S|s2cid=43750666}}</ref>
 
==Planetary system==
In 2011, 2 planets orbiting around it, were discovered, and two more suspected.<ref name=Fabrycky2011>{{citation|arxiv=1102.0543|year=2011|doi=10.1088/0067-0049/197/1/8|last1=Lissauer|first1=Jack J.|last2=Ragozzine|first2=Darin|last3=Fabrycky|first3=Daniel C.|last4=Steffen|first4=Jason H.|last5=Ford|first5=Eric B.|last6=Jenkins|first6=Jon M.|last7=Shporer|first7=Avi|last8=Holman|first8=Matthew J.|last9=Rowe|first9=Jason F.|last10=Quintana|first10=Elisa V.|last11=Batalha|first11=Natalie M.|last12=Borucki|first12=William J.|last13=Bryson|first13=Stephen T.|last14=Caldwell|first14=Douglas A.|last15=Carter|first15=Joshua A.|last16=Ciardi|first16=David|last17=Dunham|first17=Edward W.|last18=Fortney|first18=Jonathan J.|last19=Gautier, Iii|first19=Thomas N.|last20=Howell|first20=Steve B.|last21=Koch|first21=David G.|last22=Latham|first22=David W.|last23=Marcy|first23=Geoffrey W.|last24=Morehead|first24=Robert C.|last25=Sasselov|first25=Dimitar|title=Architecture and Dynamics of Kepler 'S Candidate Multiple Transiting Planet Systems|journal=The Astrophysical Journal Supplement Series|volume=197|issue=1|page=8|bibcode=2011ApJS..197....8L|s2cid=43095783}}</ref> The smaller [[Kepler-32b]], orbiting its parent star every 5.90124&nbsp;days, and [[Kepler-32c]] with an orbital period of 8.7522&nbsp;days.<ref>{{cite web|author=The Extrasolar Planet Encyclopedia|title=Kepler-32|url=http://voparis-exoplanet-new.obspm.fr/catalog/?f=%27Kepler-32%27+in+name|publisher=Exoplanet.eu|access-date=28 February 2013|url-status=dead|archive-url=https://web.archive.org/web/20140203005829/http://voparis-exoplanet-new.obspm.fr/catalog/?f=%27Kepler-32%27+in+name|archive-date=3 February 2014}}</ref> In April 2013, transit-timing variation analysis confirmed 3 other planets to be in the system. However, only very loose constraints of the maximum mass of the planets could be determined.<ref>{{Cite journal|arxiv=1201.5415|last1= Fabrycky|first1= Daniel C. |display-authors=etal.|title= Transit Timing Observations from Kepler: IV. Confirmation of 4 Multiple Planet Systems by Simple Physical Models|journal= The Astrophysical Journal|volume= 750|issue= 2|pages= 114|year= 2012|doi= 10.1088/0004-637X/750/2/114|bibcode= 2012ApJ...750..114F|s2cid= 9075167}}</ref>
In 2014, the dynamical simulation shown what the Kepler-32 planetary system have likely undergone a substantial inward migration in the past, producing an observed pattern of lower-mass planets on tightest orbits.<ref>[https://academic.oup.com/mnras/article/445/1/749/1747459 T. O. Hands, R. D. Alexander, W. Dehnen, "Understanding the assembly of Kepler's compact planetary systems", 2014]</ref> Additional yet unobserved gas giant planets on wider orbit are likely necessary for migration of smaller planets to proceed that far inward,<ref>{{citation|arxiv=1512.02649|title=There might be giants: unseen Jupiter-mass planets as sculptors of tightly-packed planetary systems|year=2015|doi=10.1093/mnras/stv2897|last1=Hands|first1=T. O.|last2=Alexander|first2=R. D.|journal=Monthly Notices of the Royal Astronomical Society|volume=456|issue=4|pages=4121–4127|doi-access=free |bibcode=2016MNRAS.456.4121H |s2cid=55175754}}</ref> although current planetary systems would be unstable if additional planets are located closer than 8.7 [[astronomical unit|AU]] from the parent star.<ref>{{citation|arxiv=1702.07714|title=Effects of Unseen Additional Planetary Perturbers on Compact Extrasolar Planetary Systems|year=2017|doi=10.1093/mnras/stx461|last1=Becker|first1=Juliette C.|last2=Adams|first2=Fred C.|journal=Monthly Notices of the Royal Astronomical Society|volume=468|issue=1|pages=549–563|doi-access=free |bibcode=2017MNRAS.468..549B|s2cid=119325005}}</ref>
 
{{OrbitboxPlanet begin
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{{Reflist|refs=
 
<ref name="Gaia DR2DR3">{{Cite Gaia DR2DR3|2080287892525359872}}</ref>
 
<ref name="McQuillan2013">{{cite journal | title=Stellar Rotation Periods of The Kepler objects of Interest: A Dearth of Close-In Planets Around Fast Rotators | last1=McQuillan | first1=A. | last2=Mazeh | first2=T. | last3=Aigrain | first3=S. | journal=The Astrophysical Journal Letters | volume=775 | issue=1 | at=L11 | year=2013 | arxiv=1308.1845 | bibcode=2013ApJ...775L..11M | doi=10.1088/2041-8205/775/1/L11 | s2cid=118557681 }}</ref>
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