Ge/Ay133

What effects do 1-10 MEarth cores have on the surrounding disk?

Today = GapsWednesday = Migration (included here)

Disks can be unstable globally:

Toomre’s criterion Q ≡ c/(Gaxisymmetric perturbations)

= epicyclic frequency

Disks can be unstable globally:

r-3 d/dr[(r2

n a Keplerian disk, where 2 = GM/r3 ,

= epicyclic frequency

S. Corder et al. 2005, OVRO

2"

AB Aur

Local resonances can propagate globally!

Linbladresonanceequations:

Inner/outertidal torque, f≈0.2 (const.)

Torque fromthe viscous disk.

Balance torques from tides and viscous response, or…

Look at time to open a gap as compared to the viscous response time scale of the disk gas. Find:

Planet mass needed to open gap:

To clear the inner disk,

How big can gaps grow?

Local resonances can propagate globally!

Gas accretion can drive global structures in the disk.

Local resonances can propagate globally!

Sufficiently large planets can create gaps, but gas accretion does continue. Can these structures assist in the formation of additional Jovian planets?

Ge/Ay133

As 1-10 MEarth cores grow and interact with the disk, what forces are involved?

Inner/outertidal torque, f≈0.2 (const.)

If the inner &outer torque arenot balanced…

The is a radial force on the planet Migration.

If you do a LINEAR analysis in a LAMINAR disk, three types of migration mechanisms emerge:

Type I – “Low mass” cores w/o an induced gap.Type II – “High mass” core with an induced gap.Type III – Runaway migration in high mass disks (really needs a non-linear analysis)

Type I:

Ward, Icarus 126, 261(1997).

Ruden review:

More on non-linear effects in a bit…

A low mass gas diskis needed to avoiddriving the cores intothe central star…

Numerically:

More on non-linear effects in a bit…

Type II:

When a gap opens,the force balancechanges. The growingplanet is now tied tothe disk transporttimescale(s). For alaminar disk:

Ward, Icarus 126, 261(1997).

Ruden review:

Recall Type I migration has

Type II versus Type I: Type II is slower, butin a linear analysis themigration rate can stillbe very fast!

Type III: With a massive disk,“runaway migration”can occur:

Very sensitive to themass surface densityprofile (can go out!).

What can we think about that might slow down migration rates?

Idea #1: Turbulent disks & stochastic migration.

Idea #2: Do not use linearity assumptions!

Non-linearities in the gas flow around an accreting protoplanet should scale as:

Where q is the secondary to primary mass ratio and h=H/r, the disk scale height/radius. In this scenario, deviations from linearity should follow:

Masset, D’Angelo & Kley (2006, ApJ, in press)

2-D and 3-D Disk simulations reveal significant non-linearity:

This can dramatically alter the outcome of migration. With sufficiently shallow mass surface density profiles the direction of migration can even be changed. (With a sufficiently shallow profile the migration is outward.)

Linear

Tests with disk viscosity.

Another interesting facet: Resonant systems migrate more slowly!

From Armitage. Why? Couple of reasons, including wider gap opening and exchange of momentum between the interacting planets & disk.

Comparison of migration predictions to observables?

The histogram data at right are from the extrasolar planet sample in Fischer & Valenti (2005) that is cut at 30 m/s for completeness. It also ignores the “hot Jupiter pile up.” The green line is the simple disk evolution model+migration.

The plot at left is a prediction that uses a simple disk evolutionary model with gas dissipation (more next time) and Type I+Type II migration.