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SUMMARY:The time evolution of the disc properties as a proxy for accretion
  models - Alice Somigliana (MPIA)
DTSTART:20260120T120000Z
DTEND:20260120T130000Z
UID:TALK243208@talks.cam.ac.uk
CONTACT:Dr Dolev Bashi
DESCRIPTION:The secular evolution of protoplanetary discs is deeply intert
 wined with both planet formation and accretion of the central protostar. P
 lanetesimals\, the building blocks of planets\, form and evolve from dust 
 grains within the disc - which follow the dynamics of the gaseous or solid
  component\, depending on their relative size\; on the other hand\, the pr
 otostar is fed by the disc itself\, through the accretion of material that
  loses angular momentum and drifts inwards. The physical mechanism driving
  accretion is still widely debated. The standard paradigm of viscous evolu
 tion prescribes a macroscopic\, turbulent viscosity as cause of a redistri
 bution of angular momentum within the disc\; however\, the observational e
 vidence of low levels of turbulence is challenging this scenario. Magnetoh
 ydrodynamic winds\, on the other hand\, prescribe material – and angular
  momentum with it – to be removed from the disc surface. Determining the
  relative contribution of the viscous and wind-driven paradigms is a compe
 lling issue\, mostly addressed looking at their impact on the observables 
 of disc populations. In this talk\, I show how the accretion model impacts
  the time evolution of (i) the disc properties-stellar mass correlations a
 nd (ii) the distribution of disc lifetimes. With a combination of disc pop
 ulation synthesis and analytical calculations\, I show that both observabl
 es trace the underlying accretion mechanism: convolving the synthetic popu
 lations with the uncertainties\, I assess the observability of the model-d
 ependent features and conclude that\, to use them as evolutionary proxies\
 , we need (i) larger samples and (ii) more accurate disc mass determinatio
 ns.\n\n
LOCATION:Ryle seminar room + ONLINE - Details to be sent by email
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