Hints for a Turnover at the Snow Line in the Giant Planet Occurrence Rate
AuthorFernandes, Rachel B.
Mulders, Gijs D.
AffiliationUniv Arizona, Lunar & Planetary Lab
planets and satellites: formation
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationRachel B. Fernandes et al 2019 ApJ 874 81
Rights© 2019. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractThe orbital distribution of giant planets is crucial for understanding how terrestrial planets form and predicting yields of exoplanet surveys. Here, we derive giant planets occurrence rates as a function of orbital period by taking into account the detection efficiency of the Kepler and radial velocity (RV) surveys. The giant planet occurrence rates for Kepler and RV show the same rising trend with increasing distance from the star. We identify a break in the RV giant planet distribution between similar to 2 and 3 au-close to the location of the snow line in the solar systemafter which the occurrence rate decreases with distance from the star. Extrapolating a broken power-law distribution to larger semimajor axes, we find good agreement with the similar to 1% planet occurrence rates from direct imaging surveys. Assuming a symmetric power law, we also estimate that the occurrence of giant planets between 0.1 and 100 au is 26.6(-5.4)(+7.5)% for planets with masses 0.1-20 M-J and decreases to 6.2(-1.2)(+1.5)% for planets more massive than Jupiter. This implies that only a fraction of the structures detected in disks around young stars can be attributed to giant planets. Various planet population synthesis models show good agreement with the observed distribution, and we show how a quantitative comparison between model and data can be used to constrain planet formation and migration mechanisms.
VersionFinal published version
SponsorsSwiss National Science Foundation [BSSGI0_155816]; NASA Science Mission directorate; National Aeronautics and Space Administration [NNX15AD94G]; NASAs Science Mission Directorate; Swiss National Science Foundation