The Formation of The Solar System Re’em Sari (Caltech) Yoram Lithwick (UCB) Peter Goldreich...
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Transcript of The Formation of The Solar System Re’em Sari (Caltech) Yoram Lithwick (UCB) Peter Goldreich...
The Formation of The Solar System
Re’em Sari (Caltech)
Yoram Lithwick (UCB)
Peter Goldreich (Caltech & IAS)
Ben Collins (Caltech)
• When did oligarchy end?• What set the number of solar system planets?• How long did it take them to form?• Why are their orbits circular and coplanar?
• Why exoplanets occupy eccentric orbits?• Why Jupiter does not!?
• What happened after planet formation?• When and how did the Oort cloud form?• How long do debris disks live?
Questions
Physical Processes: velocities
• Setup: many small bodies, few big bodies
, u , v
viscous stirring
dynamical friction
accretion
viscous stirring
collisions =
~
= solve for v
Physical Processes: accretion
• Setup: many small bodies, few big bodies
, u , v
viscous stirring
accretion
collisions =
~
Very small bodies (s«R) very fast accretion rate
~
Gravitational Instability of Particle Disk
• From Q~1:
• Required size for setup of such velocities:
€
ustab ≈πGσ
Ω≈
10 cm/s
200 cm/s
⎧ ⎨ ⎩
a ~ 1AU
a ~ 30AU
€
sstab ≈x
a
σ
ρ≈
0.2 cm
0.5 cm
⎧ ⎨ ⎩
a ~ 1AU
a ~ 30AU
Gravitational Disk Instabilities
• In very cold disk:Largest unstable wavelength
Quick collapse
No angular momentum lost
Energy dissipates by collisions€
Rmax ~ α −2 σ
ρ≈
2km
100km
a ~ 1au
a ~ 30au
⎧ ⎨ ⎩
€
S* ~ α −3 / 2 σ
ρ≈
0.05 km
2 km
a ~ 1au
a ~ 30au
⎧ ⎨ ⎩
Early Times: Runaway Accretion• Without gravitational focusing
– Bodies tend to become of equal size
• With focusing
– Few large bodies become larger than their peers.
€
1
R
dR
dt∝
1
R
€
1
R
dR
dt∝
1
R
vesc
v
⎛
⎝ ⎜
⎞
⎠ ⎟2
∝ R+1
Most of the Bodies & mass
Exponentialcutoff
Runawaytail
m
m N(m)
Late Times: Oligarchic Growth
• Big bodies heat their own food larger u around bigger bodies bigger bodies grow more slowly
big bodies are: equal mass, uniformly spaced• Number of big bodies decreases as they grow
• Super Hill - win by competition• Sub Hill - large-large accretion• Thin disk - No sustained Oligarchy
( Kokubo
and Ida
1998)
“Classical” oligarchy:
More refined oligarchy - battles:
• Formation time of Uranus & Neptune fast enough (10 Myr) if small bodies are very small (< 1 m) and very cold (e<0.05)
• In cold (sub Hill) accretion, might expect:
• Observe:
Uranus & Neptune = End of Oligarchy?
30, 000 km
20 AU 30 AUfew Hill radii
20 AU 30 AU
50, 000 km
15 Hill radii
• Formation time of earth isfast (100 Myr) even with no focusing.
• In cold accretion, might expect:
• Observed:
Earth = End of Oligarchy?
4, 000 km
0.72 AU 1 AU~3 Hill radii=0.01AU
0.72 AU 1 AU
13, 000 km
~40 Hill radii
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~30 sub-marsobjects
• Isolation when ~ • we assume u~vH
Uranus & Neptune: Beyond Isolation
50, 000 km
20 AU 30 AUfew Hill radii
• After 10 million years, • Heating > Cooling runaway heating• Planets are ejected in time
Uranus & Neptune: Ejection
50, 000 km
20 AU 30 AUfew Hill radii
• Complete N-body simulations– e.g. Kokubo & Ida (1998)
– Can not realistically treat enough small bodies.
• Statistical treatments– Interactions between mass bins
• Hybrid Codes– e.g. Kenyon
– Still difficult to have very small bodies
– Gravitational instability
• N-body + simple accretion and dynamical friction– Preliminary simulations (Collins and Sari)
Numerical Approaches
• New n-body code• Accretion• Dynamical friction
Numerical n-body Simulation
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– Contrary to current statistical models
• Extended tail up to VH
• Most of energy around VH
• Most bodies at v<<VH
Velocity Distribution
€
∂f
∂t+
r ∇v a f( ) =
∂f
∂t col
€
2 f
τ+
v
τ
∂f
∂v= − p(
r w ) f (
r v −
r w ) − f (
r v )[ ]d2w∫
Encounters within RH
Beginning of Oligarchy
• Radius of circle = Hill sphere ~ 3000R
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• Radius of circle = Hill sphere ~ 3000R
Oligarchic Growth
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End of Oligarchy
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• Radius of circle = Hill sphere ~ 3000R
• At end of oligarchy ~ , v~VH
• Only a few remaining bodies (Uranus & Neptune)• No Chaos = no heating• Cooled by remaining small bodies (explains small
eccentricity)
Uranus & Neptune: regularization
50, 000 km
20 AU 30 AU
• Vesc<Vorbit ejection unlikely
• Collisions • Formation on Geometric timescale (100 Myr)• Giant impacts!
Venus & Earth: Beyond isolation
0.72 AU 1 AU
13, 000 km
~40 Hill radii
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• When did oligarchy end?– When !! GENERAL RESULT
• What set the number of solar system planets?– Stability: No wide range chaos.
• How long did it take them to form?– About 100 Myr at a~1AU.– Faster at a~30AU !– More time until ejection at a~30AU .
• Why are their orbits circular and coplanar?– Velocity damping by small bodies.
Answers
€
=
• Small bodies:
– Inner planetary region:
• Most will be accreted.
• MMSN is sufficient!
– Outer solar system: ~5 MMSN to form Neptune.
• Large ejected bodies:
– ~3 bodies >Mearth could be in Oort cloud.
– Origin in outer planetary system.
– Survival depends on their long term stability and solar environment.
• Giant impacts:
– Expected internal to 3AU.
– Our moon
More Implications
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