Glimpsing the Compositions of Sub-Neptune-Size Exoplanets
Sub-Neptune and super-Earth sized planets are a new planet category. They account for 80% of the planet candidates discovered by *Kepler*, and 0% of the planets in the Solar System. What is the nature of these sub-Neptune-size planets, how did they form, and why are they so numerous? I will review some of the highlights from the complement of exotic sub-Neptune-size planets discovered to date and present an updated
planet mass-radius diagram, including new Keck radial velocity mass constraints for 42 small *Kepler* transiting planet candidates. From the observed planet mass-radius distribution, I'll theorize about why parts
of the distribution are unpopulated and about whether this could be a signature of planet formation and evolution. I'll focus on the intriguing transition between rocky exoplanets (comprised of iron and silicates) and planets with voluminous layers of volatiles (H/He or astrophysical ices), and explore how the current census of planets constrains this transition. Applying a hierarchical Bayesian model, I will show that the majority of 1.6 Earth-radii planets are not rocky.
|Date: ||Mardi, le 1 avril 2014|
|Lieu: ||Université McGill|
| ||Ernest Rutherford Physics Building, R.E. Bell Conference Room (room 103)|
|Contact: ||Robert Rutledge|