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SUMMARY:Predicting the Observational Signature of Migrating Neptune-sized 
 Planets in Low-viscosity Disks
DTSTART;VALUE=DATE-TIME:20200515T113000Z
DTEND;VALUE=DATE-TIME:20200515T115000Z
DTSTAMP;VALUE=DATE-TIME:20240704T115618Z
UID:indico-contribution-33@meetings.aip.de
DESCRIPTION:Speakers: Philipp Weber (Niels Bohr Institute)\nThe migration 
 of planetary cores embedded in a protoplanetary disk is an important mecha
 nism within planet-formation theory\, relevant for the architecture of pla
 netary systems. Consequently\, planet migration is actively discussed\, ye
 t often results of independent theoretical or numerical studies are uncons
 trained due to the lack of observational diagnostics designed in light of 
 planet migration. In this work we follow the idea of inferring the migrati
 on behavior of embedded planets by means of the characteristic radial stru
 ctures that they imprint in the disk’s dust density distribution. We run
  hydrodynamical multifluid simulations of gas and several dust species in 
 a locally isothermal α-disk in the low-viscosity regime (α = 10-5) and i
 nvestigate the obtained dust structures. In this framework\, a planet of r
 oughly Neptune mass can create three (or more) rings in which dust accumul
 ates. We find that the relative spacing of these rings depends on the plan
 et’s migration speed and direction. By performing subsequent radiative t
 ransfer calculations and image synthesis we show that—always under the c
 ondition of a near-inviscid disk—different migration scenarios are\, in 
 principle\, distinguishable by long-baseline\, state-of-the-art Atacama La
 rge Millimeter/submillimeter Array observations.\n\nhttps://meetings.aip.d
 e/event/1/contributions/33/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/33/
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