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SUMMARY:How super-Earths migrate in low-turbulence radiative disks - Alex 
 Ziampras (TU Munich\, Germany)
DTSTART:20241118T140000Z
DTEND:20241118T150000Z
UID:TALK222925@talks.cam.ac.uk
CONTACT:Loren E. Held
DESCRIPTION:Low-mass planets are expected to migrate in the type-I regime.
  In the inviscid limit\, the contrast between the vortensity trapped insid
 e the planet’s corotating region and the background disk leads to a dyna
 mical corotation torque\, which is thought to slow down inward migration. 
 We investigate the effect of radiative cooling on low-mass planet migratio
 n using inviscid radiation hydrodynamical simulations. We find that for in
 termediate cooling timescales (β~0.1–100)\, cooling induces a baroclini
 c forcing on material U-turning near the planet\, resulting in vortensity 
 growth in the corotating region. For longer cooling timescales\, the disk 
 buoyancy response has a similar effect. Both mechanisms in turn weaken the
  dynamical corotation torque\, are active for a substantial radial extent 
 of the disk (R∼0.1–50 au)\, and lead to significantly faster\, sustain
 ed inward migration. In the innermost few au and for super-Earth-mass plan
 ets\, which represent the bulk of the Kepler sample\, traditional type-I m
 igration gives way to nonlinear effects such as gap opening and turbulence
  induced by small-scale vortices\, with radiative cooling playing a centra
 l role in determining the fate of the planet. We finally review the effect
 s of radiation transport and discuss current challenges regarding the migr
 ation of super-Earths.
LOCATION:MR14 DAMTP and online
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