Why Do M Dwarfs Have More Transiting Planets?

We propose a planet formation scenario to explain the elevated occurrence rates of transiting planets around M dwarfs compared sun-like stars discovered by Kepler. use pebble drift and accretion model simulate growth cores inside outside snow line. A smaller size interior line delays super-Earths, allowing giant in outer disk form first. When those reach isolation mass they cut off flow pebbles inner prevent close-in super-Earths. apply this with masses between 0.1 2 solar for range initial masses. find that hot super-Earths cold are anti-correlated. The fraction our simulations is higher lower-mass matches exoplanet from forming consistent stellar dependence radial velocity surveys. key testable prediction hypothesis should decrease again near sub-stellar boundary like Trappist-1.