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SUMMARY:The effects of companions on the dynamics of protostellar discs 
 — the evolution of disc eccentricity  - Dr Enrico Ragusa - ENS de Lyon
DTSTART:20221107T140000Z
DTEND:20221107T150000Z
UID:TALK180521@talks.cam.ac.uk
CONTACT:Callum William Fairbairn
DESCRIPTION:Systems where two gravitationally bound masses (the primary ma
 ss and its companion) interact with the surrounding gas and dust are extre
 mely common in the Universe and involve a wide variety of different astrop
 hysical objects (star-star\, black hole-black hole\, star-planet\, or plan
 et-moon). The material in the surroundings of binaries is generally found 
 in a disc structure\, called “circumbinary disc”\, where the companion
  perturbative effects produce a variety of features such as: spirals\, non
 -axisymmetric overdensities\, dust/gas cavities and the evolution of the d
 isc eccentricity. \nThe great advancements during the past decade in our o
 bservational capabilities allowed us for the first time to observe such fe
 atures in protostellar discs\, triggering extensive theoretical work aimed
  at interpreting the data. \nIn this talk\, after a general overview of bi
 nary-disc interaction theory\, I will present the ongoing efforts to model
  the morphology and kinematics of protostellar discs when companions (plan
 et or stellar binaries) are present. I will discuss the current progress a
 nd highlight some open issues that still require to be addressed. In parti
 cular\, I will focus on the mutual evolution of binary/planet and disc ecc
 entricity. I will present numerical simulations and novel results in this 
 context showing that the tidal truncation efficiency of binaries appears t
 o increase in eccentric discs. I will discuss the possible relevance of th
 is effect for interpreting the observations of protostellar discs with cav
 ities. I will finally spend a few words about the importance of bridging t
 he gap between theory and observations by providing the observational comm
 unity with ready to use theoretical results in the form of synthetic obser
 vations.
LOCATION:In Person MR14
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