Planet occurrence within 0.25AU of solar-type stars from Kepler
Article
Article Title | Planet occurrence within 0.25AU of solar-type stars from Kepler |
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ERA Journal ID | 1058 |
Article Category | Article |
Authors | Howard, Andrew W. (Author), Marcy, Geoffrey W. (Author), Bryson, Stephen T. (Author), Jenkins, Jon M. (Author), Rowe, Jason F. (Author), Batalha, Natalie M. (Author), Borucki, William J. (Author), Koch, David G. (Author), Dunham, Edward W. (Author), Gautier, Thomas N. (Author), Van Cleve, Jeffrey (Author), Cochran, William D. (Author), Latham, David W. (Author), Lissauer, Jack J. (Author), Torres, Guillermo (Author), Brown, Timothy M. (Author), Gilliland, Ronald L. (Author), Buchhave, Lars A. (Author), Caldwell, Douglas A. (Author), Christensen-Dalsgaard, Jorgen (Author), Ciardi, David (Author), Fressin, Francois (Author), Haas, Michael R. (Author), Howell, Steve B. (Author), Kjeldsen, Hans (Author), Seager, Sara (Author), Rogers, Leslie (Author), Sasselov, Dimitar D. (Author), Steffen, Jason H. (Author), Basri, Gibor S. (Author), Charbonneau, David (Author), Christiansen, Jessie (Author), Clarke, Bruce (Author), Dupree, Andrea (Author), Fabrycky, Daniel C. (Author), Fischer, Debra A. (Author), Ford, Eric B. (Author), Fortney, Jonathan J. (Author), Tarter, Jill (Author), Girouard, Forrest R. (Author), Holman, Matthew J. (Author), Johnson, John Asher (Author), Klaus, Todd C. (Author), MacHalek, Pavel (Author), Moorhead, Althea V. (Author), Morehead, Robert C. (Author), Ragozzine, Darin (Author), Tenenbaum, Peter (Author), Twicken, Joseph D. (Author), Quinn, Samuel N. (Author), Isaacson, Howard (Author), Shporer, Avi (Author), Lucas, Philip W. (Author), Walkowicz, Lucianne M. (Author), Welsh, William F. (Author), Boss, Alan (Author), DeVore, Edna (Author), Gould, Alan (Author), Smith, Jeffrey C. (Author), Morris, Robert L. (Author), Prsa, Andrej (Author), Morton, Timothy D. (Author), Still, Martin (Author), Thompson, Susan E. (Author), Mullally, Fergal (Author), Endl, Michael (Author) and MacQueen, Phillip J. (Author) |
Journal Title | Astrophysical Journal Supplement Series |
Journal Citation | 201 (2), pp. 15-34 |
Article Number | 15 |
Number of Pages | 20 |
Year | 2012 |
Publisher | IOP Publishing |
Place of Publication | United States |
ISSN | 0067-0049 |
1538-4365 | |
Digital Object Identifier (DOI) | https://doi.org/10.1088/0067-0049/201/2/15 |
Web Address (URL) | http://iopscience.iop.org/article/10.1088/0067-0049/201/2/15 |
Abstract | We report the distribution of planets as a function of planet radius, orbital period, and stellar effective temperature for orbital periods less than 50days 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 ⊕. 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 /a. We consid'r first Kepler target stars within the 'solar subset' having T eff = 4100-6100K, 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 ⊕. 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 ⊕) and out to the longest orbital period (50days, 0.25AU) in our study. For P < 50 days, the distribution of planet radii is given by a power law, df/dlog R = kRR α with kR = 2.9+0.5 - 0.4, α = -1.92 ± 0.11, and R ≡ R p/R ⊕. 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 2days are extremely rare; for R p > 2 R ⊕ we measure an occurrence of less than 0.001 planets per star. For all planets with orbital periods less than 50days, 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 ⊕, 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 3600-7100K, spanning M0 to F2 dwarfs. Over this range, the occurrence of 2-4 R ⊕ planets in the Kepler field increases with decreasing T eff, with these small planets being seven times more abundant around cool stars (3600-4100K) than the hottest stars in our sample (6600-7100K). |
Keywords | planetary systems; stars; photometric; |
Contains Sensitive Content | Does not contain sensitive content |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
Public Notes | For access to this article, please click on the URL link provided. |
Institution of Origin | University of Southern Queensland |
Byline Affiliations | University of California, United States |
NASA Ames Research Center, United States | |
SETI Institute, United States | |
San Jose University, United States | |
Lowell Observatory, United States | |
California Institute of Technology (Caltech), United States | |
University of Texas at Austin, United States | |
Center for Astrophysics Harvard and Smithsonian, United States | |
Las Cumbres Observatory, United States | |
Space Telescope Science Institute, United States | |
University of Copenhagen, Denmark | |
Aarhus University, Denmark | |
National Aeronautics and Space Administration (NASA), United States | |
National Optical Astronomy Observatory, United States | |
Massachusetts Institute of Technology, United States | |
Fermilab Cosmic Physics Centre, United States | |
Massey University, New Zealand | |
University of Florida, United States | |
University of Hertfordshire, United Kingdom | |
San Diego State University, United States | |
Carnegie Institution of Washington, United States | |
Lawrence Hall of Science, United States | |
Villanova University, United States |
https://research.usq.edu.au/item/q4321/planet-occurrence-within-0-25au-of-solar-type-stars-from-kepler
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