Terrestrial planet formation across the galaxy Sean Raymond - PowerPoint PPT Presentation

Migration stops at the inner edge of the disk Masset et al (2006)

A type 1 migration map Cossou et al 2014; see also Lyra et al 2010, Paardekooper et al 2011; Kretke & Lin 2012; Horn et al 2012; Coleman & Nelson 2014; and especially Bitsch et al 2013, 2014ab, 2015

A type 1 migration map Cossou et al 2014; see also Lyra et al 2010, Paardekooper et al 2011; Kretke & Lin 2012; Horn et al 2012; Coleman & Nelson 2014; and especially Bitsch et al 2013, 2014ab, 2015

A type 1 migration map Cossou et al 2014; see also Lyra et al 2010, Paardekooper et al 2011; Kretke & Lin 2012; Horn et al 2012; Coleman & Nelson 2014; and especially Bitsch et al 2013, 2014ab, 2015

A type 1 migration map Cossou et al 2014; see also Lyra et al 2010, Paardekooper et al 2011; Kretke & Lin 2012; Horn et al 2012; Coleman & Nelson 2014; and especially Bitsch et al 2013, 2014ab, 2015

A type 1 migration map Cossou et al 2014; see also Lyra et al 2010, Paardekooper et al 2011; Kretke & Lin 2012; Horn et al 2012; Coleman & Nelson 2014; and especially Bitsch et al 2013, 2014ab, 2015

A type 1 migration map Cossou et al 2014; see also Lyra et al 2010, Paardekooper et al 2011; Kretke & Lin 2012; Horn et al 2012; Coleman & Nelson 2014; and especially Bitsch et al 2013, 2014ab, 2015

A type 1 migration map Cossou et al 2014; see also Lyra et al 2010, Paardekooper et al 2011; Kretke & Lin 2012; Horn et al 2012; Coleman & Nelson 2014; and especially Bitsch et al 2013, 2014ab, 2015

Cossou, Raymond et al 2014

Cossou, Raymond et al 2014

Resonant chains usually go unstable as or after gas disk dissipates Instability Resonant chain 3:25:4 4:35:4 3:2 2:1 4:3 7:6 Migration during 3 Myr gas disk lifetime Cossou, Raymond et al 2014

Resonant chains usually go unstable as or after gas disk dissipates Most hot super-Earths that form by Instability Resonant chain migration do not remain in resonant 3:25:4 chains (Terquem & Papaloizou 2007; Goldreich & Schlichting 4:35:4 3:2 2014; Cossou et al 2014) 2:1 4:3 7:6 Migration during 3 Myr gas disk lifetime Cossou, Raymond et al 2014

Why no hot super-Earths in Solar System?

Why no hot super-Earths in Solar System? • Fast-forming gas giants can act as a barrier to inward-migrating super-Earths (Izidoro et al 2015)

Why no hot super-Earths in Solar System? • Fast-forming gas giants can act as a barrier to inward-migrating super-Earths (Izidoro et al 2015)

Why no hot super-Earths in Solar System? • Fast-forming gas giants can act as a barrier Prediction: systems of hot super-Earths should be anti-correlated with giant planets to inward-migrating super-Earths (Izidoro et al on more distant (1-5 AU) orbits 2015)

Solar System

Solar System The “small Mars” problem

Solar System The “small Mars” problem Grand Tack model: Jupiter, Saturn migrated inward then back outward

Solar Angry gas System giants The “small Mars” problem Grand Tack model: Jupiter, Saturn migrated inward then back outward

Solar Angry gas System giants The “small Mars” Migration: terrestrial problem planets form WET Grand Tack model: Jupiter, Saturn migrated inward then back outward

Solar Angry gas System giants The “small Mars” Migration: terrestrial problem planets form WET Grand Tack model: Planet-planet Jupiter, Saturn scattering can destroy migrated inward then terrestrial planets back outward

Solar Hot super- Angry gas System Earths giants The “small Mars” Migration: terrestrial problem planets form WET Grand Tack model: Planet-planet Jupiter, Saturn scattering can destroy migrated inward then terrestrial planets back outward

Solar Hot super- Angry gas System Earths giants The “small Mars” May form by inward Migration: terrestrial problem migration of planetary planets form WET embryos Grand Tack model: Planet-planet Jupiter, Saturn scattering can destroy migrated inward then terrestrial planets back outward