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SUMMARY:Kinematics and dynamics of self-gravitating protostellar discs - C
 ristiano Longarini (Institute of Astronomy\, Cambridge)
DTSTART:20241125T140000Z
DTEND:20241125T150000Z
UID:TALK222928@talks.cam.ac.uk
CONTACT:Thomas Jannaud
DESCRIPTION:Protoplanetary discs are the link between stars and planet: th
 ey form with the star\, and they are the environments where planet formati
 on takes place. Nowadays\, thanks to the incredible images of ALMA (Atacam
 a Large Millimetre Array)\, we have the possibility to investigate planet 
 formation in real time. ALMA observations show that planet formation is ub
 iquitous\, and occurs very early in the disc lifetime\, when the disc is s
 till massive. In such massive environments\, gravitational instabilities a
 re likely to occur\, playing a crucial role in disc evolution. In this sem
 inar\, I will discuss the kinematical and dynamical effects of self-gravit
 y and gravitational instability in protoplanetary discs.\nFrom a kinematic
 al perspective\, disc self-gravity alters the equilibrium state\, producin
 g a super-Keplerian rotation curve. Measuring this deviation allows us to 
 constrain key properties of protoplanetary discs\, such as their mass. Mor
 eover\, gravitational instabilities leave distinct kinematic signatures\, 
 observable with ALMA\, that provide crucial insights into angular momentum
  transport in these systems. I will illustrate these concepts by comparing
  theoretical predictions with ALMA observations of two protoplanetary disc
 s likely to exhibit gravitational instabilities.\nSecondly\, I will explor
 e the process of planet formation in gravitationally unstable discs. Speci
 fically\, I will highlight how the interplay with dust dynamics enables th
 e formation of planetary cores via dust collapse in the outer disc regions
 . This mechanism bypasses the planetesimal formation barrier within the co
 re accretion model of planet formation. I will present hydrodynamical simu
 lations demonstrating dust collapse in gas spiral arms and examine the ear
 ly evolution of the resulting planetary cores.
LOCATION:MR14 DAMTP and online
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