BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//CERN//INDICO//EN
BEGIN:VEVENT
SUMMARY:Evolution and growth of dust grains in protoplanetary disks with m
 agnetically driven disk wind
DTSTART;VALUE=DATE-TIME:20200513T091000Z
DTEND;VALUE=DATE-TIME:20200513T093000Z
DTSTAMP;VALUE=DATE-TIME:20240704T115619Z
UID:indico-contribution-42@meetings.aip.de
DESCRIPTION:Speakers: Tetsuo Taki (National Astronomical Observatory of Ja
 pan)\nMagnetically driven disk winds (MDWs) are one of the promising mecha
 nisms of dispersal processes of protoplanetary disks (Suzuki et al. 2010\,
  Bai 2013). When the MDWs play a key role\, the gaseous component of proto
 planetary disks evolves in a different manner from that of the classical v
 iscous evolution. As a result\, the subsequent planet formation is also af
 fected by the MDWs. In this work\, we investigate the effects of the MDWs 
 on the radial drift of solid particles with a size of 0.1$\\mu$m - 1km. We
  propose that the MDWs is a possible solution to the ``radial drift barrie
 r'' of collisionally growing dust grains\, which is a severe obstacle to t
 he planet formation (e.g.\, Nakagawa et al.1986).\nIn order to study the e
 volution of dust grains in the disks\, we calculate the advection and coll
 isional growth of dust particles in evolving protoplanetary disks under th
 e 1+1 D (time + radial distance) approximation. We solve a coagulation equ
 ation of solid particles under a single-size approximation (Sato et al. 20
 16) for various conditions of turbulent viscosity\, the mass loss by the M
 DW\, and the magnetic braking by the MDW.\nWe found that significant grain
  growth occurs in the inner region of the protoplanetary disks. The grown 
 dust particles are larger than the km-sized bodies and they are no longer 
 caught by the radial drift barrier. The mechanism of such successful dust 
 growth is separated into two parts: (1) the increase of the equilibrium si
 ze of the dust particles caused by the convergent flow of the dust mass an
 d dispersal of the gas component\, (2) the unstable dust growth driven by 
 the feedback loop between the size\, radial drift velocity\, and surface d
 ensity of the dust component. The disk evolution owing to the MDWs strongl
 y supports the former part of the growth mechanism. When the equilibrium s
 ize of the dust particles reaches the size that the Stokes number of the d
 ust particles exceeds unity\, the dust size evolution shift to the unstabl
 e mode (i.e.\, the latter part).\nBecause of the successful growth of dust
  particles\, the ring-like structure containing the planetesimal sized bod
 ies can be formed at the inner part of the protoplanetary disks. We will d
 iscuss the effects of such the ring-like structure on the subsequent plane
 tary system formation and the disk observations.\n\nhttps://meetings.aip.d
 e/event/1/contributions/42/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/42/
END:VEVENT
END:VCALENDAR