BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//Talks.cam//talks.cam.ac.uk//
X-WR-CALNAME:Talks.cam
BEGIN:VEVENT
SUMMARY:What dust sizes tell us about planet-forming disc evolution - Fran
 cesco Zagaria (University of Cambridge)
DTSTART:20220216T131500Z
DTEND:20220216T134500Z
UID:TALK170414@talks.cam.ac.uk
CONTACT:Hannah Uebler
DESCRIPTION:Protoplanetary discs are the birthplace of planets: knowledge 
 of their evolution mechanism is key to understand how planet formation tak
 es place and to explain the properties of the currently detected exoplanet
 s. Traditionally\, planet-forming discs have been thought to evolve viscou
 sly: angular momentum redistribution allows for accretion and leads to out
 ward disc spreading. Recently\, it was hypothesised instead that accretion
  is due to angular momentum removal by MHD winds\, implying that no disc s
 preading is expected. We run several 1D gas and dust simulations of viscou
 s and MHD discs with the aim of assessing which evolution mechanism is the
  dominant one. To do so\, we compute disc dust sizes and compare them with
  ALMA observations. We show that viscous and MHD angular momentum transpor
 t determine very different dust disc sizes. In particular\, MHD models are
  compact\, as expected from the bulk of the data\, while in viscous models
  dust sizes increase with time. However\, current observations lack enough
  sensitivity to discriminate between the two evolutionary scenarios. Deepe
 r ALMA observation could be helpful to assess the dominant evolution mecha
 nisms of planet-forming discs.
LOCATION:The Hoyle Lecture Theatre + Zoom 
END:VEVENT
END:VCALENDAR