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SUMMARY:Investigating a new paradigm for type II migration
DTSTART;VALUE=DATE-TIME:20200513T072500Z
DTEND;VALUE=DATE-TIME:20200513T074500Z
DTSTAMP;VALUE=DATE-TIME:20240704T115619Z
UID:indico-contribution-60@meetings.aip.de
DESCRIPTION:Speakers: Dylan Kloster (OCA)\nUnderstanding the origins and d
 ynamics of massive planets during the planet-formation process is essentia
 l to understanding how the structures of individual planetary systems came
  to be.  Massive planets have the ability to open gaps in their host disk\
 , and the radial movements of these gap-opening planets is typically refer
 red to as type II migration.  In the classical view\, a protoplanetary dis
 k accretes onto its star on a viscous timescale\, carrying this gap inward
 s with the planet moving with the gap.  This theory assumes that the plane
 t remains in a state of quasi-equilibrium at the center of the gap. Howeve
 r\, a non-zero torque from the disk must be applied to the planet for it t
 o move radially\, meaning the planet is not necessarily located at equilib
 rium.  This implies that while the gap is in motion\, and the planet is be
 ing dragged along with it\, the location of the planet is not necessarily 
 at the center of the gap.  In addition\, if we define the location of the 
 gap center to be the radial position of a planet with a fixed orbit (i.e.\
 , a non-migrating planet)\, we also consider the possibility that the equi
 librium position of the planet differs from this center.  We explore these
  properties involving the gap-planet interaction of an evolving protoplane
 tary disk with 2D simulations using the FargOCA hydrodynamics code.  We ac
 complish this by fixing the orbital radius of a massive planet ($M_p/M_* =
  0.001$) until its disk has reached a steady state.  At this stage we rele
 ase the planet from its fixed orbit\, and allow it to migrate freely.  We 
 then analyze the planet's displacement from equilibrium\, as well as its d
 isplacement from the gap center\, varying disk properties such as aspect r
 atio and viscosity\, and explore their effects on the planet migration rat
 e.\n\nhttps://meetings.aip.de/event/1/contributions/60/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/60/
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