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

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Terrestrial planet formation across the galaxy Sean Raymond Laboratoire dAstrophysique de Bordeaux planetplanet.net Image credit: NASA/Ames/JPL-Caltech Collaborators Alessandro Morbidelli Franck Selsis (Bordeaux) (Nice)

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SLIDE 1

Terrestrial planet formation across the galaxy

Sean Raymond Laboratoire d’Astrophysique de Bordeaux planetplanet.net

Image credit: NASA/Ames/JPL-Caltech

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SLIDE 2

Collaborators

  • Alessandro Morbidelli

(Nice)

  • Andre Izidoro (Bordeaux)
  • Arnaud Pierens (Bordeaux)
  • Kevin Walsh (SwRI)
  • Avi Mandell (NASA

Goddard)

  • Emeline Bolmont (Namur)
  • Nate Kaib (Carnegie)
  • Tom Quinn (U. Washington)
  • Jonathan Lunine (Cornell)
  • Franck Selsis (Bordeaux)
  • Christophe Cossou

(Bordeaux)

  • Dave O’Brien (PSI)
  • Phil Armitage (U. Colorado)
  • Rory Barnes (U.

Washington)

  • Seth Jacobson (Nice)
  • Mark Wyatt (Cambridge)
  • Amaya Moro-Martin (StSci)
  • Bertram Bitsch (Lund)
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SLIDE 3

Stages of Planet Formation

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SLIDE 4

Stages of Planet Formation

Grains

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SLIDE 5

Stages of Planet Formation

Grains Planetesimals

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SLIDE 6

Stages of Planet Formation

Grains Planetesimals Planetary Embryos

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SLIDE 7

Stages of Planet Formation

Grains Planetesimals Planetary Embryos

while gas remains

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SLIDE 8

Stages of Planet Formation

Grains Planetesimals Planetary Embryos

while gas remains

Type 1 migration

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SLIDE 9

Stages of Planet Formation

Grains Planetesimals Planetary Embryos

while gas remains

Gaseous Planets

Type 1 migration

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SLIDE 10

Stages of Planet Formation

Grains Planetesimals Planetary Embryos

while gas remains

Gaseous Planets

Type 2 migration Type 1 migration

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SLIDE 11

Stages of Planet Formation

Grains Planetesimals

No more gas

Planetary Embryos

while gas remains

Gaseous Planets

Type 2 migration Type 1 migration

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SLIDE 12

Stages of Planet Formation

Grains Planetesimals

No more gas

Planetary Embryos

while gas remains

Gaseous Planets

Type 2 migration Type 1 migration Dynamical instabilities

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SLIDE 13

Stages of Planet Formation

Grains Planetesimals

No more gas

Planetary Embryos

while gas remains

Gaseous Planets Terrestrial Planets

Type 2 migration Type 1 migration Dynamical instabilities

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SLIDE 14

Stages of Planet Formation

Grains Planetesimals

No more gas

Planetary Embryos

while gas remains

Gaseous Planets Terrestrial Planets

Type 2 migration Type 1 migration Dynamical instabilities

INFLUENCE

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SLIDE 15

Stages of Planet Formation

Grains Planetesimals

No more gas

Planetary Embryos

while gas remains

Gaseous Planets Terrestrial Planets

Type 2 migration Type 1 migration Dynamical instabilities

INFLUENCE

Debris disks

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SLIDE 16
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SLIDE 17

Most stars have planets

(e.g., Cassan et al 2012)

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SLIDE 18

>15%

(Cumming et al 2008; Gould et al 2010; Mayor et al 2011)

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SLIDE 19

>15%

(Cumming et al 2008; Gould et al 2010; Mayor et al 2011)

10%

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SLIDE 20

>15%

(Cumming et al 2008; Gould et al 2010; Mayor et al 2011)

90% 10%

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SLIDE 21

>15%

(Cumming et al 2008; Gould et al 2010; Mayor et al 2011)

90% 10% <85%

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SLIDE 22

>15%

(Cumming et al 2008; Gould et al 2010; Mayor et al 2011)

90% 10% <85% 30-50+% of all stars

(Mayor et al 2011, Howard et al 2010, 2012)

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SLIDE 23

>15%

(Cumming et al 2008; Gould et al 2010; Mayor et al 2011)

90% 10% <85% 30-50+% of all stars

(Mayor et al 2011, Howard et al 2010, 2012)

Solar System(-like)

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SLIDE 24

>15%

(Cumming et al 2008; Gould et al 2010; Mayor et al 2011)

90% 10% <85% 30-50+% of all stars

(Mayor et al 2011, Howard et al 2010, 2012)

Angry gas giants Solar System(-like)

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SLIDE 25

>15%

(Cumming et al 2008; Gould et al 2010; Mayor et al 2011)

90% 10% <85% 30-50+% of all stars

(Mayor et al 2011, Howard et al 2010, 2012)

Angry gas giants Solar System(-like) “Hot super-Earths”

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SLIDE 26

Formation of the inner Solar System

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Gas giants on circular orbits

Raymond, Quinn & Lunine 2006

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Gas giants on circular orbits

Raymond, Quinn & Lunine 2006

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SLIDE 29

Wetherill 1991; Chambers 2001; O’Brien et al 2006; Raymond et al 2006, 2009, Morishima et al 2008, 2010; Nagasawa et al 2005, 2007; Thommes et al 2008; Fischer & Ciesla 2014; Izidoro et al 2014

Raymond et al 2009

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SLIDE 30

Wetherill 1991; Chambers 2001; O’Brien et al 2006; Raymond et al 2006, 2009, Morishima et al 2008, 2010; Nagasawa et al 2005, 2007; Thommes et al 2008; Fischer & Ciesla 2014; Izidoro et al 2014

The “small Mars” Problem

Raymond et al 2009

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SLIDE 31

A possible solution to the small Mars problem

(Hansen 2009; also Wetherill 1978; Chambers 2001)

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A possible solution to the small Mars problem

(Hansen 2009; also Wetherill 1978; Chambers 2001)

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SLIDE 33

A possible solution to the small Mars problem

(Hansen 2009; also Wetherill 1978; Chambers 2001)

  • A small Mars forms

naturally if inner disk is

  • nly from 0.7-1 AU
  • An edge effect

Hansen 2009, ApJ, 703, 1131

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A possible solution to the small Mars problem

(Hansen 2009; also Wetherill 1978; Chambers 2001)

  • A small Mars forms

naturally if inner disk is

  • nly from 0.7-1 AU
  • An edge effect

Hansen 2009, ApJ, 703, 1131

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SLIDE 35

Time Semi major axis Jupiter

~50 MEarth Type II migration starting ~ 200 MEarth

Jupiter in the gaseous disk

slide by Kevin Walsh

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Time Semi major axis Jupiter Saturn

~50 MEarth Fast Migration Capture in Resonance

Jupiter and Saturn in the gaseous disk

slide by Kevin Walsh

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Time Semi major axis Jupiter Saturn

Capture in Resonance

Gas disk starts to dissipate

Jupiter and Saturn in the gaseous disk

slide by Kevin Walsh Masset & Snellgrove 2001; Morbidelli & Crida 2007; Pierens & Nelson 2008; Crida et al 2009; Pierens & Raymond 2011; Pierens et al 2014

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Hydrodynamical simulation

(Pierens & Raymond 2011; Masset & Smellgrove 2001)

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SLIDE 39

Hydrodynamical simulation

(Pierens & Raymond 2011; Masset & Smellgrove 2001)

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The Grand Tack model

Walsh, Morbidelli, Raymond, O’Brien, Mandell 2011, Nature, 475, 206

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The Grand Tack model

Walsh, Morbidelli, Raymond, O’Brien, Mandell 2011, Nature, 475, 206

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SLIDE 42

Walsh et al 2011, Nature, 475, 206

The Grand Tack

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Water is delivered to Earth by same population that was implanted into asteroid belt as C types

(Walsh et al 2011; O’Brien et al 2014)

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Water is delivered to Earth by same population that was implanted into asteroid belt as C types

(Walsh et al 2011; O’Brien et al 2014)

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SLIDE 45

The Grand Tack terrestrial planets

Walsh et al 2011; Morbidelli et al 2012; O’Brien et al, 2014; Raymond et al 2014; Jacobson et al 2014; Jacobson & Morbidelli 2014; Raymond & Morbidelli 2014; Jacobson & Walsh 2015.

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SLIDE 46

Terrestrial planet formation with angry gas giants

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SLIDE 47

Giant exoplanets

Wright et al 2011

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SLIDE 48

Giant exoplanets

Wright et al 2011

  • rbital migration
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Giant exoplanets

Wright et al 2011

  • rbital migration

planet-planet scattering

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Mandell, Raymond & Sigurdsson 2007

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Mandell, Raymond & Sigurdsson 2007

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Raymond, Mandell & Sigurdsson 2006

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Raymond, Mandell & Sigurdsson 2006

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SLIDE 54

Credit: Nahks Tr’Enhl

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Planet-planet scattering

Credit: Eric Ford

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SLIDE 56

Raymond et al 2012; see also talk by A. Mustill

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SLIDE 57

Raymond et al 2012; see also talk by A. Mustill

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SLIDE 58

Formation

  • f systems
  • f hot

super-Earths

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SLIDE 59

Hot Super Earths

Raymond et al 2014 PP6 chapter; Kepler data from Batalha et al 2013 and Rowe et al 2014

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SLIDE 60

Hot Super Earths

Raymond et al 2014 PP6 chapter; Kepler data from Batalha et al 2013 and Rowe et al 2014

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SLIDE 61

Orbital distance

Hot super- Earths

1-4 REarth Size

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Orbital distance

Hot super- Earths

  • 1. In-situ

accretion 1-4 REarth Size

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SLIDE 63

Orbital distance

Hot super- Earths

  • 1. In-situ

accretion 1-4 REarth

  • 2. Radial (aerodynamic) drift

Size

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SLIDE 64

Orbital distance

Hot super- Earths

  • 1. In-situ

accretion

  • 3. Inward (type 1) migration

1-4 REarth

  • 2. Radial (aerodynamic) drift

Size

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In-situ accretion: planets form fast in high-mass disks

Bolmont, Raymond et al 2014 ~15 ME in inside 0.5 AU

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Gas disk lifetime

Planets that form in-situ should migrate

See also Inamdar & Schlichting 2015, Ogihara et al 2015; Grishin & Perets 2015

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SLIDE 67

Gas disk lifetime

Planets that form in-situ should migrate

If hot super-Earths form in-situ then they must interact strongly with gaseous disk

See also Inamdar & Schlichting 2015, Ogihara et al 2015; Grishin & Perets 2015

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SLIDE 68

Gas disk lifetime

Planets that form in-situ should migrate

If hot super-Earths form in-situ then they must interact strongly with gaseous disk Because they must migrate, hot super-Earths can’t form “in-situ”!

See also Inamdar & Schlichting 2015, Ogihara et al 2015; Grishin & Perets 2015

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Orbital distance Mass

Forming hot super-Earths by type 1 migration

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Orbital distance Mass

Forming hot super-Earths by type 1 migration

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SLIDE 71

Orbital distance Mass

Forming hot super-Earths by type 1 migration

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Type 1 migration

  • Inward or
  • utward
  • Timescale

~10-100 kyr (bigger=faster)

Golreich & Tremaine 1980; Ward 1986, 1997; Tanaka et al 2002; Kley & Crida 2008; Paardekooper et al 2010, 2011; Pierens et al 2013; Lega et al 2014; Bitsch et al 2014

Credit: A. Pierens

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SLIDE 73

Armitage 2011

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SLIDE 74

Masset et al (2006)

Migration stops at the inner edge of the disk

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Masset et al (2006)

Migration stops at the inner edge of the disk

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Masset et al (2006)

Migration stops at the inner edge of the disk

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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

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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

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SLIDE 79

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

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SLIDE 80

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

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SLIDE 81

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

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SLIDE 82

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

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SLIDE 83

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

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SLIDE 84

Cossou, Raymond et al 2014

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SLIDE 85

Cossou, Raymond et al 2014

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Resonant chains usually go unstable as or after gas disk dissipates

Cossou, Raymond et al 2014 7:6 4:3 2:1 3:2 4:35:4 3:25:4 Resonant chain Instability Migration during 3 Myr gas disk lifetime

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SLIDE 87

Resonant chains usually go unstable as or after gas disk dissipates

Cossou, Raymond et al 2014 7:6 4:3 2:1 3:2 4:35:4 3:25:4 Resonant chain Instability

Most hot super-Earths that form by migration do not remain in resonant chains (Terquem & Papaloizou 2007; Goldreich & Schlichting

2014; Cossou et al 2014) Migration during 3 Myr gas disk lifetime

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SLIDE 88

Why no hot super-Earths in Solar System?

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SLIDE 89

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)

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SLIDE 90

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)

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SLIDE 91

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)

Prediction: systems of hot super-Earths should be anti-correlated with giant planets

  • n more distant (1-5 AU) orbits
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SLIDE 92
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SLIDE 93

Solar System

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SLIDE 94

Solar System

The “small Mars” problem

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SLIDE 95

Solar System

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

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SLIDE 96

Angry gas giants Solar System

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

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SLIDE 97

Angry gas giants

Migration: terrestrial planets form WET

Solar System

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

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SLIDE 98

Angry gas giants

Migration: terrestrial planets form WET Planet-planet scattering can destroy terrestrial planets

Solar System

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

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SLIDE 99

Angry gas giants

Migration: terrestrial planets form WET Planet-planet scattering can destroy terrestrial planets

Solar System

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

Hot super- Earths

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SLIDE 100

Angry gas giants

Migration: terrestrial planets form WET Planet-planet scattering can destroy terrestrial planets

Solar System

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

Hot super- Earths

May form by inward migration of planetary embryos

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SLIDE 101

Angry gas giants

Migration: terrestrial planets form WET Planet-planet scattering can destroy terrestrial planets

Solar System

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

Hot super- Earths

May form by inward migration of planetary embryos Jupiter: a barrier for inward-migrating super-Earths?

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SLIDE 102

Orbital distance Mass

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Orbital distance Mass

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SLIDE 104

Orbital distance Mass

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SLIDE 105

Orbital distance Mass

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SLIDE 106

Orbital distance Mass

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SLIDE 107

Orbital distance Mass

The Grand Tack

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Orbital distance Mass

The Grand Tack

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Orbital distance Mass

Planet-planet scattering

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  • The “small Mars” problem and the Grand Tack:
  • Raymond et al (2009, Icarus)
  • Walsh et al (2011, Nature)
  • Effect of “angry” gas giants:
  • Raymond et al (2006, Science)
  • Raymond et al (2011, 2012, A&A)
  • Formation of hot super-Earths:
  • Raymond et al (2008, MNRAS; 2014, PP6)
  • Cossou et al (2014, A&A)
  • Izidoro et al (2015, ApJ Letters)
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Extra Slides

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SLIDE 112

S-type C-type

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SLIDE 113
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SLIDE 114
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SLIDE 115
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SLIDE 116
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The late veneer as a clock for the Moon-forming impact

Jacobson, Morbidelli, Raymond, O’Brien, Walsh, Rubie 2014, Nature

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The outer Solar System

Planetesimals in movie are 100m; Raymond et al in prep

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SLIDE 119

The outer Solar System

Planetesimals in movie are 100m; Raymond et al in prep

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SLIDE 120

Raymond et al 2011

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SLIDE 121

Raymond et al 2011

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SLIDE 122

Large oscillations in e, i (“Generalized Milankovitch cycles”): impact on climate

47

Spiegel, Raymond et al 2010

Green = habitable Red = freezing Blue = supercold Key fact: orbit-averaged flux increases with e as (1-e2)-1/2

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SLIDE 123

Large oscillations in e, i (“Generalized Milankovitch cycles”): impact on climate

47

Spiegel, Raymond et al 2010

Green = habitable Red = freezing Blue = supercold Key fact: orbit-averaged flux increases with e as (1-e2)-1/2

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SLIDE 124

Orbital distance Mass

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SLIDE 125

Orbital distance Mass

slide-126
SLIDE 126

Orbital distance Mass

slide-127
SLIDE 127

Orbital distance Mass

slide-128
SLIDE 128

Orbital distance Mass

slide-129
SLIDE 129

Orbital distance Mass

slide-130
SLIDE 130

Orbital distance Mass

The Grand Tack

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SLIDE 131

Orbital distance Mass