Skip to main content
SearchLoginLogin or Signup

Understanding the High Occurrence Rate of Hot Sub-Neptunes at Young and Intermediate Ages

Presentation #402.06 in the session 0, 2, 3, N Stars.

Published onApr 03, 2024
Understanding the High Occurrence Rate of Hot Sub-Neptunes at Young and Intermediate Ages

Recent demographics results from TESS and K2 have revealed that stars in young (< 100 My) and intermediate age (< 1 Gyr) clusters have a significantly higher occurrence rate of hot sub-Neptunes than older (3-9 Gyr) field stars. In this talk, we compare those results to the predicted effects of planet evolution, migration, and cluster environment. For planet evolution, the currently understood timescales of photoevaporation (< 100 My) and core-powered mass loss (0.5-2 Gy), posited to explain the dearth of planets between 1.5 and 2 Earth radii, are well separated, and amenable to testing with occurrence rates in young clusters. However, migration (including disk-driven and secular migration) timescales are not dissimilar and cannot be easily disentangled. In addition, the cluster environment in which the planets are formed may impact the resulting observed population, through both radiation and dynamical effects. We discuss these competing processes and their expected timescales and impacts, and highlight what we can learn from current observations. Finally, we outline upcoming opportunities to observationally test the impacts of these effects, and further clarify the broader picture of early planetary system formation and evolution.

Comments
0
comment
No comments here