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SUMMARY:Modelling the Emission from Winds from Photoevaporating Protoplane
 tary Discs  - Andrew Sellek (Cambridge)
DTSTART:20221011T120000Z
DTEND:20221011T130000Z
UID:TALK183158@talks.cam.ac.uk
CONTACT:Dr Emily Sandford
DESCRIPTION:Several processes – including accretion of material onto the
  central star\, planet formation\, and winds – all contribute to dispers
 ing protoplanetary discs within the first few millions theirs of their hos
 t star’s lifetime. To date\, however\, observations have not been able t
 o conclusively quantify the contribution of winds. I will discuss two mode
 lling efforts to predict emission from winds and how this might be used to
  learn about their launching mechanisms. Firstly\, the MIRI instrument of 
 JWST may be able to resolve the emission from atomic forbidden lines in th
 e infrared\, allowing us to constrain the heating and ionisation of the ou
 tflowing material. Using simple prescriptions for a photoevaporative wind 
 structure\, we can cheaply explore the parameter space to discover which p
 arts of the winds this emission probes and what its morphology might revea
 l about their nature. Secondly\, winds that effectively remove material fr
 om the outermost regions of protoplanetary discs are also induced by nearb
 y massive stars\; this material\, however\, does not have a homogeneous co
 mposition due to molecular freeze out and transport on dust grains. Using 
 a 1D disc evolution code we are exploring when this leads to winds with de
 pleted metal abundances and the potential consequences for observing wind 
 emission and hence constraining disc dispersal by external photoevaporatio
 n. 
LOCATION:Ryle seminar room + ONLINE - Details to be sent by email
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