BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//Talks.cam//talks.cam.ac.uk//
X-WR-CALNAME:Talks.cam
BEGIN:VEVENT
SUMMARY:Dust dynamics during a protostellar collapse: analytical and numer
 ical multifluid methods. - Gabriel Verrier (CEA Saclay\, France)
DTSTART:20251015T130000Z
DTEND:20251015T140000Z
UID:TALK237715@talks.cam.ac.uk
CONTACT:Thomas Jannaud
DESCRIPTION:Dust grains are key players of the evolution of the dense inte
 rstellar medium. The grain size distribution varies locally\, modifying th
 e thermodynamics and the chemistry of molecular clouds\, the opacity of co
 llapsing protostellar cores and the coupling between the gas and the magne
 tic field\, and the solid content to form planetesimals in protoplanetary 
 disks. Magnetohydrodynamical models are commonly used to study the formati
 on of stars and disks\, but they generally do not capture the complexity o
 f the interactions with the dusty component.\n\nThis complexity requires a
 nalytical and numerical methods that offer complementary levels of detail.
  In the first part of the talk\, I present a multifluid approach that mode
 ls the dynamics of a dust size distribution in interaction with the gas an
 d the magnetic field. We explore its fundamental physics in the linear reg
 ime. We discuss the consequences of the coupling of the dust with the magn
 etic field on dust enrichment within the protostellar envelope and on magn
 etic braking (Verrier et al\, in prep). In a second part of the talk\, I p
 resent our new multifluid numerical method that allows us to simulate 3D d
 usty protostellar collapses (Verrier et al\, 2025). This method is designe
 d to capture all the coupling regimes between the gas and the neutral dust
  grains\, including the terminal velocity regime (Lebreuilly et al\, 2019)
 . We find that millimeter dust grains enrich the first hydrostatic core an
 d some locations of the envelope\, promoted by the initial turbulence of t
 he dense core\, setting favourable conditions to early planet formation sc
 enarios. Finally\, we present perspectives that connect dust dynamics in t
 urbulence and dust growth.
LOCATION:MR14 DAMTP and online
END:VEVENT
END:VCALENDAR