Planetary Science Seminar Winter-2018

Sub-Neptunes around FGKM dwarfs are evenly distributed in log period down to ~10 days but dwindle in number at shorter orbital periods. I will demonstrate how magnetospheric truncation of disks and tidal inspiral of planets are responsible for sculpting this orbital architecture. Both the break at ~10 days and the slope of the occurrence rate down to ~1 day can be reproduced if planets form in disks that are truncated by their host star magnetospheres at co-rotation. Planets can be brought from disk edges to ultra-short (<1 day) periods by tides raised on their stars. Tidal migration can explain why these ultra-short period planets (USPs) are more widely spaced than their longer period counterparts. Planets around metal-rich stars occupy a wider range of orbital periods and planetary radii. I will discuss how pre-main sequence stellar evolution and the evolution of solid disks can give rise to the diversity of planets seen around metal-rich stars.