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SUMMARY:Protoplanetary disc: what can we learn by combining theory and obs
 ervations? - Claudia Toci (ESO)
DTSTART:20240227T130000Z
DTEND:20240227T140000Z
UID:TALK210829@talks.cam.ac.uk
CONTACT:Dr Emily Sandford
DESCRIPTION:Protoplanetary discs serve as the cradle for planetary formati
 on and evolution. It is then fundamental to study their evolution to gain 
 a comprehensive understanding of exoplanetary system formation. These disc
 s can be studied using two distinct approaches.\n\nOn one side\, they can 
 be analysed as a set of single sources\, allowing for a detailed analysis 
 of the mechanisms behind the diversity of observed morphologies using gas 
 and dust tracers such as rings\, gaps and asymmetries.\n\nOn the other sid
 e\, it is crucial to study star-forming regions\, understanding which phys
 ical processes are governing the global disc evolution. \n\n \n\nIn this t
 alk\, I will firstly describe results from the modelling of single sources
 \, underlining the information we can obtain by comparing multi-wavelength
 s observations with results from the hydrodynamical models of specific sou
 rces (e.g.\, HD169142\, PDS70\, GG Tau A). In particular\, I will focus on
  how simulations can help in constraining the mass and position of the can
 didate proto-planets that may be responsible for the ALMA and SPHERE obser
 vational results\, as well as how they can support future observational st
 rategies. \n\n \n\nI will then summarize some of the results obtained by t
 esting disc evolution models by comparing them with the Lupus star forming
  region. In these works\, we tested the secular evolution of the observed 
 dust and gas radius of disc populations and their ratio\, to test the effi
 ciency of radial drift and the viscous evolution theory.
LOCATION:Ryle seminar room + ONLINE - Details to be sent by email
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