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SUMMARY:Non-equilibrium dynamics of massive embedded planetary systems
DTSTART;VALUE=DATE-TIME:20200513T124500Z
DTEND;VALUE=DATE-TIME:20200513T130500Z
DTSTAMP;VALUE=DATE-TIME:20240704T115619Z
UID:indico-contribution-52@meetings.aip.de
DESCRIPTION:Speakers: Thomas Rometsch (University of Tübingen)\nRecently\
 , young planets with masses around $10\\\,M_\\text{Jupiter}$ which are sti
 ll embedded in a disk have been observed\, e.g. in the PDS 70 system. At t
 his mass range\, the planet-disk interaction is non-linear and the planets
  are attributed with having carved the observed gap into their parent disk
 . One possible scenario for the formation of large gaps is outward migrati
 on in 2:1 mean motion resonance (MMR) where the inner planet is more massi
 ve than the outer one. This process is known to strongly excite the planet
 s' eccentricities which in turn leads to eccentric gaps. The latter could 
 be an observable feature of such systems. \n\nWe perform 2D\, vertically i
 ntegrated hydrodynamics simulations to study the migration and dynamics of
  the embedded planetary system employing a viscous $\\alpha$-disk model. T
 o avoid artificial wave-damping boundary conditions we choose large outer 
 disk radii and work in the center of mass frame of the planetary system. I
 n addition to the often used locally isothermal equation of state\, we run
  simulations with radiative cooling\, viscous heating and irradiation from
  the star from which temperature distributions in the perturbed disk can b
 e extracted.\n\nThe simulations exhibit the expected smooth 2:1 MMR outwar
 d migration. For sufficiently high surface densities of the order of the m
 inimum mass solar nebula we additionally observe epochs of fast migration.
  During a sequence which we call migration jumps\, the outer planet underg
 oes fast outward migration traveling tens of au outward. It stays at the l
 arge distance for some kyr before returning back into the 2:1 MMR via fast
  inward migration. The whole sequence only takes 10-20 kyr. Meanwhile the 
 inner planet remains relatively unaffected. A migration jump causes strong
  perturbations in the disk including pronounced spiral arms and asymmetric
  features including vortices and mass accumulation in the Lagrange points 
 inside the gap region. The latter might be an observational indication for
  this process.\n\nDue to the large mass of the embedded planets\, the feat
 ures created in the disk are strong and synthetic observations of the simu
 lations might help to identify whether these mechanisms are at play in the
  disks we observe. In addition\, migration jumps of massive planets can be
  expected to cause strong scattering of dust particles and small bodies in
  the radial range on which the jumps occur. Thereby\, they might play an i
 mportant role for the dust and small body distribution in the earlier stag
 es of the systems lifetime.\n\nhttps://meetings.aip.de/event/1/contributio
 ns/52/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/52/
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