Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 479, Issue 4, Pages 5012-5021Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/sty1760
Keywords
planets and satellites: dynamical evolution and stability; planets and satellites: formation
Categories
Funding
- Royal Society University Research Fellowship
- NASA [NNX14AP31G]
- NSF [AST1715246]
- National Aeronautics and Space Administration under the Exoplanet Exploration Program
- NASA [NNX14AP31G, 675330] Funding Source: Federal RePORTER
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The mass-period or radius-period distribution of close-in exoplanets shows a paucity of intermediate mass/size (sub-Jovian) planets with periods less than or similar to 3 d. We show that this sub-Jovian desert can be explained by the photoevaporation of highly irradiated sub-Neptunes and the tidal disruption barrier for gas giants undergoing high-eccentricity migration. The distinctive triangular shape of the sub-Jovain desert results from the fact that photoevaporation is more effective closer to the host star, and that in order for a gas giant to tidally circularize closer to the star without tidal disruption it needs to be more massive. Our work indicates that super-Earths/mini-Neptunes and hot-Jupiters had distinctly separate formation channels and arrived at their present locations at different times.
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