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Viewing Solar System Architecture Through an Extrasolar Lens - - PowerPoint PPT Presentation
Viewing Solar System Architecture Through an Extrasolar Lens - - PowerPoint PPT Presentation
Viewing Solar System Architecture Through an Extrasolar Lens Konstantin Batygin (Caltech) Greg Laughlin (UC Santa Cruz) Planets with known masses Jupiters ! (10% of Sun-like stars) Hot Jupiters ! (1% of Sun-like stars) Planets with known
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Hot Jupiters ! (1% of Sun-like stars) Jupiters ! (10% of Sun-like stars)
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Planets with known radii
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Hot Jupiters (1% of Sun-like stars) Close-in sub-Jovian planets (50% of Sun-like stars)
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Jupiter Saturn Neptune Earth Mercury
1 R
- Kepler Planet Candidates (sub-Jovian)
100R
r = log10 ✓ a R ◆
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Jupiter Mars Earth Venus Mercury
single planet systems 2 planet systems 3 planet systems 4+ planet systems
Saturn Neptune Earth Mercury
1 R
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Minimum Mass Solar Nebula
(Hayashi 1981)
Σ = 1700 ⇣ a 1AU ⌘−1.5 g/cm2
fdust ∼ 1.5% fdust ∼ 0.5%
a < 2.7AU a > 2.7AU
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Minimum Mass Solar Nebula
(Hayashi 1981)
Minimum Mass Extrasolar Nebula
(Chiang & Laughlin 2013)
Σ = 1700 ⇣ a 1AU ⌘−1.5 g/cm2
Σ ∼ 104 ⇣ a 1AU ⌘−1.6 g/cm2 fdust ∼ 0.5% fdust ∼ 1.5% fdust ∼ 0.5%
a < 2.7AU a > 2.7AU
gas solid
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Relative to other Sun-like, planet-bearing stars, the Solar system’s terrestrial region is severely depleted in mass.
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Relative to other Sun-like, planet-bearing stars, the Solar systems’ terrestrial region is severely depleted in mass.
Our proposition: Long-range (a few AU) migration of Jupiter in the Solar nebula Orbital excitation of planetesimals by resonant sweeping Destructive collisional cascade and removal by aerodynamic drift Resonant shepherding of close-in planets by drifting debris
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3:2 resonant lock established
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Jupiter’s inward trek resonantly sweeps up planetesimals
planetesimals + gas
Jupiter
2:1 MMR
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Jupiter’s inward trek resonantly sweeps up planetesimals
planetesimals + gas
Jupiter
2:1 MMR
√a h 1 − p 1 − e2 i = const.
Adiabatic invariance dictates excitation of orbital eccentricity
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time (years) planetesimal - Jupiter period ratio B
2:1 MMR 3:2 1:1
- utward scattering
resonant capture and transport
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semi-major axis (AU)
- rbital eccentricity
Jupiter’s orbital migration
A
100 km planetesimals
resonant transport
- u
t w a r d s c a t t e r i n g unswept disk 2:1 resonance
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semi-major axis (AU)
- rbital eccentricity
Jupiter’s orbital migration
A
10 km planetesimals
resonant transport
- utward scattering
unswept disk 2:1 resonance
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semi-major axis (AU)
- rbital eccentricity
Jupiter’s orbital migration
A
1000 km planetesimals
r e s
- n
a n t t r a n s p
- r
t
- u
t w a r d s c a t t e r i n g unswept disk 2:1 resonance
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Jupiter
2:1 MMR
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Jupiter
2:1 MMR planetesimals
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ν ⇠ n σ v = Mtot/m 2πhei tanhiia3 πs2vKhei ~ a collision every ~20 orbits
Jupiter
2:1 MMR planetesimals
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Collisions can lead to fragmentation accretion
- r
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Collisions are catastrophic if:
✓m0 M ◆ ✓v2
enc
2 ◆ > 1 2ρ ✓ R 1 cm ◆1.36
(Leinhardt & Stewart 2009)
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Collisions are catastrophic if:
✓m0 M ◆ ✓v2
enc
2 ◆ > 1 2ρ ✓ R 1 cm ◆1.36
3 g/cm3 (rock) 10,100,1000 km
∼ e vkep impactor-target mass ratio of ~10% yields fragmentation!
(Leinhardt & Stewart 2009)
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Jupiter’s migration shepherds planetesimals inwards and grinds them down to smaller sizes
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vgas = vK s 1 − 3 c2
s
v2
K
ˆ ϕ = vK(1 − η) ˆ ϕ adrag = −π CD 2m s2ρgasvrelvrel.
~0.005
Gas is sub-Keplerian small (<1km) planetesimals feel a head-wind Aerodynamics
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time (years)
- rbital radius (AU)
- rbital decay of a putative Kepler-11 system under the
influence of a drifting population of 100m planetesimals
b c d e g f
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Jupiter’s current orbit is a consequence of inward-outward migration, facilitated by a resonance with Saturn
Summary
The inward phase of Jupiter’s migration entrained planetesimals into interior resonances and led to orbital excitation The resulting collisional avalanche generated a debris disk that would have aerodynamically driven any pre-existing short planets into the Sun
Jupiter’s orbital migration resonant transport- u
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