Planet Occurrence within 0.25 AU of Solar-Type Stars from Kepler

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dc.contributor.utaustinauthorCochran, William D.en_US
dc.contributor.utaustinauthorEndl, Michaelen_US
dc.contributor.utaustinauthorMacQueen, Phillip J.en_US
dc.creatorHoward, Andrew W.en_US
dc.creatorMarcy, Geoffrey W.en_US
dc.creatorBryson, Stephen T.en_US
dc.creatorJenkins, Jon M.en_US
dc.creatorRowe, Jason F.en_US
dc.creatorBatalha, Natalie M.en_US
dc.creatorBorucki, William J.en_US
dc.creatorKoch, David G.en_US
dc.creatorDunham, Edward W.en_US
dc.creatorGautier, Thomas N., IIIen_US
dc.creatorVan Cleve, Jeffreyen_US
dc.creatorCochran, William D.en_US
dc.creatorLatham, David W.en_US
dc.creatorLissauer, Jack J.en_US
dc.creatorTorres, Guillermoen_US
dc.creatorBrown, Timothy M.en_US
dc.creatorGilliland, Ronald L.en_US
dc.creatorBuchhave, Lars A.en_US
dc.creatorCaldwell, Douglas A.en_US
dc.creatorChristensen-Dalsgaard, Jorgenen_US
dc.creatorCiardi, Daviden_US
dc.creatorFressin, Francoisen_US
dc.creatorHaas, Michael R.en_US
dc.creatorHowell, Steve B.en_US
dc.creatorKjeldsen, Hansen_US
dc.creatorSeager, Saraen_US
dc.creatorRogers, Leslieen_US
dc.creatorSasselov, Dimitar D.en_US
dc.creatorSteffen, Jason H.en_US
dc.creatorBasri, Gibor S.en_US
dc.creatorCharbonneau, Daviden_US
dc.creatorChristiansen, Jessieen_US
dc.creatorClarke, Bruceen_US
dc.creatorDupree, Andreaen_US
dc.creatorFabrycky, Daniel C.en_US
dc.creatorFischer, Debra A.en_US
dc.creatorFord, Eric B.en_US
dc.creatorFortney, Jonathan J.en_US
dc.creatorTarter, Jillen_US
dc.creatorGirouard, Forrest R.en_US
dc.creatorHolman, Matthew J.en_US
dc.creatorJohnson, John Asheren_US
dc.creatorKlaus, Todd C.en_US
dc.creatorMachalek, Pavelen_US
dc.creatorMoorhead, Althea V.en_US
dc.creatorMorehead, Robert C.en_US
dc.creatorRagozzine, Darinen_US
dc.creatorTenenbaum, Peteren_US
dc.creatorTwicken, Joseph D.en_US
dc.creatorQuinn, Samuel N.en_US
dc.creatorIsaacson, Howarden_US
dc.creatorShporer, Avien_US
dc.creatorLucas, Philip W.en_US
dc.creatorWalkowicz, Lucianne M.en_US
dc.creatorWelsh, William F.en_US
dc.creatorBoss, Alanen_US
dc.creatorDevore, Ednaen_US
dc.creatorGould, Alanen_US
dc.creatorSmith, Jeffrey C.en_US
dc.creatorMorris, Robert L.en_US
dc.creatorPrsa, Andrejen_US
dc.creatorMorton, Timothy D.en_US
dc.creatorStill, Martinen_US
dc.creatorThompson, Susan E.en_US
dc.creatorMullally, Fergalen_US
dc.creatorEndl, Michaelen_US
dc.creatorMacQueen, Phillip J.en_US
dc.date.accessioned2016-10-28T19:35:25Z
dc.date.available2016-10-28T19:35:25Z
dc.date.issued2012-08en_US
dc.description.abstractWe report the distribution of planets as a function of planet radius, orbital period, and stellar effective temperature for orbital periods less than 50 days around solar-type (GK) stars. These results are based on the 1235 planets (formally "planet candidates") from the Kepler mission that include a nearly complete set of detected planets as small as 2 R-circle plus. For each of the 156,000 target stars, we assess the detectability of planets as a function of planet radius, R-p, and orbital period, P, using a measure of the detection efficiency for each star. We also correct for the geometric probability of transit, R-star/a. We consider first Kepler target stars within the "solar subset" having T-eff = 4100-6100 K, log g = 4.0-4.9, and Kepler magnitude Kp < 15 mag, i.e., bright, main-sequence GK stars. We include only those stars having photometric noise low enough to permit detection of planets down to 2 R-circle plus. We count planets in small domains of R-p and P and divide by the included target stars to calculate planet occurrence in each domain. The resulting occurrence of planets varies by more than three orders of magnitude in the radius-orbital period plane and increases substantially down to the smallest radius (2 R-circle plus) and out to the longest orbital period (50 days, similar to 0.25 AU) in our study. For P < 50 days, the distribution of planet radii is given by a power law, df/d log R = k(R)R(alpha) with k(R) = 2.9(-0.4)(+0.5), alpha = -1.92 +/- 0.11, and R equivalent to R-p/R-circle plus. This rapid increase in planet occurrence with decreasing planet size agrees with the prediction of core-accretion Formation but disagrees with population synthesis models that predict a desert at super-Earth and Neptune sizes for close-in orbits. Planets with orbital periods shorter than 2 days are extremely rare; for R-p > 2 R-circle plus we measure an occurrence of less than 0.001 planets per star. For all planets with orbital periods less than 50 days, we measure occurrence of 0.130 +/- 0.008, 0.023 +/- 0.003, and 0.013 +/- 0.002 planets per star for planets with radii 2-4, 4-8, and 8-32 R-circle plus, in agreement with Doppler surveys. We fit occurrence as a function of P to a power-law model with an exponential cutoff below a critical period P-0. For smaller planets, P-0 has larger values, suggesting that the "parking distance" for migrating planets moves outward with decreasing planet size. We also measured planet occurrence over a broader stellar T-eff range of 3600-7100 K, spanning M0 to F2 dwarfs. Over this range, the occurrence of 2-4 R-circle plus planets in the Kepler field increases with decreasing T-eff, with these small planets being seven times more abundant around cool stars (3600-4100 K) than the hottest stars in our sample (6600-7100 K).en_US
dc.description.departmentAstronomyen_US
dc.description.sponsorshipNASA NNX06AH52Gen_US
dc.description.sponsorshipNational Center for Atmospheric Researchen_US
dc.description.sponsorshipNational Science Foundationen_US
dc.description.sponsorshipNASA's Science Mission Directorateen_US
dc.identifierdoi:10.15781/T2CJ87P1C
dc.identifier.citationHoward, Andrew W., Geoffrey W. Marcy, Stephen T. Bryson, Jon M. Jenkins, Jason F. Rowe, Natalie M. Batalha, William J. Borucki et al. "PLANET OCCURRENCE WITHIN 0.25 AU OF SOLAR-TYPE STARS FROM KEPLER Based in part on observations obtained at the WM Keck Observatory, which is operated by the University of California and the California Institute of Technology." The Astrophysical Journal Supplement Series, Vol. 201, No. 2 (Aug., 2012): 15.en_US
dc.identifier.doi10.1088/0067-0049/201/2/15en_US
dc.identifier.issn0067-0049en_US
dc.identifier.urihttp://hdl.handle.net/2152/42972
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.relation.ispartofserialAstrophysical Journal Supplement Seriesen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.rights.restrictionOpenen_US
dc.subjectplanetary systemsen_US
dc.subjectstars: statisticsen_US
dc.subjecttechniques: photometricen_US
dc.subjectneptune-mass planeten_US
dc.subjectsuper-earthen_US
dc.subjectextrasolar planetsen_US
dc.subjecthot jupitersen_US
dc.subjectdeterministic modelen_US
dc.subjecttransiting planeten_US
dc.subjectlow-densityen_US
dc.subjectradiusen_US
dc.subjectrelationshipsen_US
dc.subjectterrestrial planetsen_US
dc.subjectsolid exoplanetsen_US
dc.subjectastronomy & astrophysicsen_US
dc.titlePlanet Occurrence within 0.25 AU of Solar-Type Stars from Kepleren_US
dc.typeArticleen_US

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