TIC low mass stars radius

The slope is consistent, within 0.3{sigma}, with those around Sun-like stars. For M dwarfs, the discrepancy is 3.6{sigma} with the extrapolated slope from the Kepler FGK sample, marking the point where the deviation from previous results begins. Moreover, we do not see a clear shift in the radius valley between early and mid M dwarfs.

The flatter scaling of the radius valley for lower-mass stars suggests that mechanisms other than atmospheric mass loss through photoevaporation may shape the radius distribution of planets around M dwarfs. A comparison of the slope with various planet formation and evolution models leads to a good match with pebble accretion models including water worlds, indicating a potentially different regime of planet formation that can be probed with exoplanets around the lowest-mass stars.