BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//CERN//INDICO//EN
BEGIN:VEVENT
SUMMARY:Constraining the Radial Turbulence Parameter $\\alpha$ from the Di
 stribution of Water and Refractory species in an Evolving Solar Nebula
DTSTART;VALUE=DATE-TIME:20200511T121500Z
DTEND;VALUE=DATE-TIME:20200511T123500Z
DTSTAMP;VALUE=DATE-TIME:20241101T160705Z
UID:indico-contribution-5-53@meetings.aip.de
DESCRIPTION:Speakers: Anusha Kalyaan (Clemson University)\nThe overall str
 ucture of the evolving protoplanetary disk is set by the interaction of ac
 cretion and dispersal processes such as turbulence\, winds and photoevapor
 ation (Ercolano & Pascucci 2017)\, with finer structural details (as gaps\
 , cavities\, spirals and warps) in the disk provided by planet formation (
 eg. Van der Marel et al. 2015). Recent meteoritic evidence from Kruijer et
  al. (2017) strongly suggest the presence of two distinct isotopic reservo
 irs in the \n\nhttps://iaus379.aip.de/event/1/contributions/53/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://iaus379.aip.de/event/1/contributions/53/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Are Protoplanetary Disks Truly Laminar?
DTSTART;VALUE=DATE-TIME:20200511T115000Z
DTEND;VALUE=DATE-TIME:20200511T121000Z
DTSTAMP;VALUE=DATE-TIME:20241101T160705Z
UID:indico-contribution-5-28@meetings.aip.de
DESCRIPTION:Speakers: Jacob Simon (Iowa State University)\nRecent years ha
 ve seen tremendous progress in our understanding of angular momentum trans
 port in protoplanetary disks.  It is now thought that accretion is driven 
 primarily by a large-scale vertical field threading the disk\, either thro
 ugh magnetically launched winds or large-scale magnetic stresses within th
 e disk plane.  However\, it remains an open question as to just how lamina
 r these accreting disks are.  Even if not the primary source of angular mo
 mentum transport\, turbulence may still play a crucial role in the multitu
 de of processes involved in forming planets. \n\nIn this talk\, I will pre
 sent both theoretical and observational evidence that protoplanetary disks
  are not necessarily laminar and in some cases can still harbor vigorous t
 urbulence.   From ALMA observations of molecular line broadening\, we now 
 know of at least one source that presents a clear signature of turbulence.
   I will present these compelling new observations and compare them to ear
 lier predictions of magnetically driven turbulence. I will also present a 
 number of numerical experiments that indeed show magnetically driven turbu
 lence is still present throughout large regions of the disk\, even in the 
 presence of a large-scale magnetic field.  I will conclude with an outlook
  for future observational and theoretical studies and what the results so 
 far imply for our understanding of planet formation and disk evolution.\n\
 nhttps://iaus379.aip.de/event/1/contributions/28/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://iaus379.aip.de/event/1/contributions/28/
END:VEVENT
BEGIN:VEVENT
SUMMARY:A systematic exploration of magnetised disc wind solutions in prot
 oplanetary discs
DTSTART;VALUE=DATE-TIME:20200511T112500Z
DTEND;VALUE=DATE-TIME:20200511T114500Z
DTSTAMP;VALUE=DATE-TIME:20241101T160705Z
UID:indico-contribution-5-20@meetings.aip.de
DESCRIPTION:Speakers: Geoffroy Lesur (Institute of planetology and astroph
 ysics of Grenoble/CNRS)\nThe recent developments in our understanding of t
 he chemical composition\, the ionisation equilibrium and the dynamics of p
 rotoplanetary discs has led to the conclusion that magnetised disc wind (M
 DW) are probably playing an important role in shaping the long term evolut
 ion of these objects. Most of our understanding of these winds comes from 
 global direct numerical simulations which include complex microphysics and
  which explore only a very limited subspace of parameters. Hence\, it is v
 ery difficult to draw firm conclusions about the long-term evolution of di
 scs subject to MDW. \n\nIn this contribution\, I will present a systematic
  exploration of MDW solutions\, which can then be used in secular models t
 o predict the evolution of a disc\, in a way similar to the "alpha disc" m
 odel. I will also discuss the solutions topology (top/down symmetry\, midp
 lane/surface accretion layers\, laminar stress\, etc...) which have often 
 been mis-interpreted in the literature.\n\nhttps://iaus379.aip.de/event/1/
 contributions/20/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://iaus379.aip.de/event/1/contributions/20/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Magnetic flux transport in protoplanetary discs
DTSTART;VALUE=DATE-TIME:20200511T110000Z
DTEND;VALUE=DATE-TIME:20200511T112000Z
DTSTAMP;VALUE=DATE-TIME:20241101T160705Z
UID:indico-contribution-5-27@meetings.aip.de
DESCRIPTION:Speakers: Philip Leung ()\nMagnetic effects are important for 
 accretion disc dynamics. In PPDs\, much still needs to be understood in ho
 w non-ideal MHD effects (Ohmic\, Hall and ambipolar diffusion)\, which are
  relevant because of the low ionisation levels found in much of the disc\,
  affect the radial accumulation and retention of magnetic flux needed for 
 processes such as the launching of a magnetic disc wind. I aim to present 
 results from semi-analytic local models incorporating all three non-ideal 
 effects\, and how they inform our understanding of the flux transport prob
 lem. I will also be presenting some recent numerical simulations exploring
  the interplay of these non-ideal effects with the magnetic field geometry
 \, and the resulting implications on the flux transport process.\n\nhttps:
 //iaus379.aip.de/event/1/contributions/27/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://iaus379.aip.de/event/1/contributions/27/
END:VEVENT
END:VCALENDAR