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SUMMARY:Giant planet migration in low-viscosity disks
DTSTART;VALUE=DATE-TIME:20200513T122000Z
DTEND;VALUE=DATE-TIME:20200513T124000Z
DTSTAMP;VALUE=DATE-TIME:20240704T115619Z
UID:indico-contribution-40@meetings.aip.de
DESCRIPTION:Speakers: Alessandro Morbidelli (OCA)\nGiant planet migration 
 (a.k.a. Type-II migration) should occur with a migration speed proportiona
 l to the disk's viscosity. This has been verified for alpha-disks with alp
 ha>1.e-4 (Robert et al.\, 2018). But what happens in disks with vanishing 
 viscosity? Does Type-II migration stalls? A variety of behaviors have been
  observed in the literature for migration in low-viscosity disks. Migratio
 n seems to be very stochastic\, with very fast migration episodes (e.g. Mc
 Nally et al.\, 2018).   However\, most simulations so far have been conduc
 ted in 2D disks. We find that low-viscosity 3D disks are much more stable 
 than 2D disks of equivalent viscosity when they are perturbed by a planet\
 , because they are submitted to the constraint of vertical hydrostatic equ
 ilibrium. Consequently giant planet migration in 3D disks behaves more reg
 ularly. Nevertheless\, the presence of vortex formed at the outer edge of 
 the gap opened by the planet affects the planet evolution. We have investi
 gated in details the influence of a vortex on planet migration and on the 
 growth of the planet's orbital eccentricity as well as the feedback of the
  eccentricity on migration.\n\nhttps://meetings.aip.de/event/1/contributio
 ns/40/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/40/
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