Detection and Characterization of Jovian Planets

Mass-period distribution

Dependence on
the stellar [Fe/H]

Dependence on M*

Multiple systems

Planetary interior:
diverse structure & Fe/H

Avenues of planet formation

Disk evolution

Inner disks disappear ~ 10 Myr

Potential observational signatures

Condensation sequence

Signs of Crystalline grains

Slide 13

Chondritic meteorites

From dust to planetesimals

From planetesimals to embryos

Growth during gas depletion

Disk-planet tidal interactions

Competition: M growth & a decay

Embryos’ type I migration (10 Mearth)

(Mass) growth vs (orbital) decay

Preferred cradles of gas giants: snow line

Accretion onto cores

Giant impacts

Flow into the Roche lobe

Effect of type I migration

The period distribution:
Type II migration

short-period cutoff

Stellar metallicity, mass loss, & circularization of hot Jupiters

Transits: atmosphere & structure

period cutoffs

The mass distribution

Metallicity dependence

Stellar mass-metallicity

Multiple planets

Migration-free sweeping secular resonances

Dynamical shake up (Nagasawa, Thommes)

Migration, Collisions, & damping

Giant impact & lunar formation

Sweeping clear of planetesimals

Last melting events of chondrules

Sweeping secular resonance in ESP’s

Formation of warm Neptunes

Post Depletion Dynamical  Stability

Mean motion resonance capture

A 2 Mearth “hot rock” planet in a 7-d orbit observed for 6 months with APF @ 1.3 m/s precision

Frequency of Earth

1 Mearth planet in a 35-d habitable-zone orbit
 around a nearby M dwarf – observed for 6 months with a 9-telescope global array @ 2.0 m/s precision

Sequential accretion scenario summary

Outstanding issues: