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SUMMARY:Winds in transition disks
DTSTART;VALUE=DATE-TIME:20200515T093500Z
DTEND;VALUE=DATE-TIME:20200515T095500Z
DTSTAMP;VALUE=DATE-TIME:20240704T115536Z
UID:indico-contribution-7-61@meetings.aip.de
DESCRIPTION:Speakers: Étienne Martel (IPAG)\nProtoplanetary disks (PPD) h
 ave been widely observed around young stars and are supposed to host plane
 tary formation. Among these disks stand the transition disks (TD) which ar
 e characterized by a large hole in the central regions\, whose formation r
 emains yet unexplained. Despite this hole\, accretion rates comparable to 
 the ones found in PPD are measured\, suggesting an inward motion of matter
 .\n\nA possible explanation for these high accretion rates is the presence
  of magnetised winds that would allow matter to fall onto the star at high
  radial velocity. Following previous works\, the disk can be described usi
 ng non ideal MHD while the ideal MHD picture is used to compute the wind.\
 n\nI will show the impact of the depleted dust repartition in TDs on the i
 onization fraction through theoretical calculations based on a simple latt
 ice of chemical reactions. It can be shown that the non ideal MHD effects 
 are also affected by such a hole.  I will then present the results of 2D s
 imulations modelling winds in a TD based on the predicted non ideal effect
 s profiles.\n\nAxisymetry allows to explore the parameters space and to ch
 eck the stability of the hole profile through time. Such a work will later
  on lead the way to a more accurate description of the chemistry at stake 
 in TD and 3D simulations.\n\nhttps://meetings.aip.de/event/1/contributions
 /61/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/61/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The time variable dynamics of snow-lines
DTSTART;VALUE=DATE-TIME:20200515T091000Z
DTEND;VALUE=DATE-TIME:20200515T093000Z
DTSTAMP;VALUE=DATE-TIME:20240704T115536Z
UID:indico-contribution-7-31@meetings.aip.de
DESCRIPTION:Speakers: James Owen (Imperial College London)\nSnow-lines are
  regions of protoplanetary discs where volatiles transition from the solid
 -phase to the gas phase. They play an important role in the chemical evolu
 tion of protoplanetary discs and perhaps planet/planetesimal formation. Th
 e majority of work treats these transitions as passive\, uncoupled from th
 e dynamics. I will argue that snow-lines in the outer regions of protoplan
 etary discs (where the dis cooling is optically thin)\, are thermally unst
 able. Namely\, condensation leads to an increase in the solid abundance wh
 ich leads to increased cooling and more condensation (or vica-versa). I wi
 ll demonstrate a dynamical simulation that actively couples the condensati
 on physics\, to the radiative transfer and hence the disc's temperature\, 
 dust dynamics and growth. I will use this simulation to show that snow-lin
 es are not static\, but dynamically evolve in otherwise stationary discs a
 nd drive the dynamics in the outer regions of protoplanetary discs. We fin
 d the CO snow-line can move 10s AU on timescales of a few 1e5 years\, crea
 ting further structures and rings in the disc and even multiple snow-lines
 . This thermal instability at snow-lines is likely important for the chemi
 cal\, thermal and dynamical evolution of protoplanetary discs. It perhaps 
 even plays a role in explaining ringed ALMA discs and planet/planetesimal 
 formation.\n\nhttps://meetings.aip.de/event/1/contributions/31/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/31/
END:VEVENT
BEGIN:VEVENT
SUMMARY:What are the dynamical signatures of vortices?
DTSTART;VALUE=DATE-TIME:20200515T084500Z
DTEND;VALUE=DATE-TIME:20200515T090500Z
DTSTAMP;VALUE=DATE-TIME:20240704T115536Z
UID:indico-contribution-7-59@meetings.aip.de
DESCRIPTION:Speakers: Heloise Meheut (UCA/CNRS)\nThe large scale crescent 
 shape structures detected in protoplanetary disks have sometimes been inte
 rpreted as vortices. Vortices are of particular interest to understand pla
 net formation as they are known to concentrate dust and could participate 
 to planetesimal formation. We study the multiple fingerprints of such larg
 e Rossby vortices and propose observational predictions to test the if the
 se crescents could be interpreted as vortices.\n\nWe performed 2D hydro-si
 mulations where a vortex forms at the edge of a gas depleted region. We de
 rived idealized line-of-sight velocity maps\, varying orientation relative
  to the observer. The signal of interest\, as a small perturbation to the 
 dominant axisymetric component in velocity\, may be isolated in observatio
 nal data using a proxy for the dominant quasi-Keplerian velocity. We propo
 se that the velocity curve on the observational major axis be such a proxy
 . Applying our method to the disk around HD 142527 as a study case\, we pr
 edict line-of-sight velocities scarcely detectable by currently available 
 facilities. We show that corresponding spirals patterns can also be detect
 ed with similar spectral resolutions.\n\nhttps://meetings.aip.de/event/1/c
 ontributions/59/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/59/
END:VEVENT
BEGIN:VEVENT
SUMMARY:An Origin of Misaligned Disks and Planetary Orbits: Angular Moment
 um Accretion in Star Formation Process
DTSTART;VALUE=DATE-TIME:20200515T075000Z
DTEND;VALUE=DATE-TIME:20200515T081000Z
DTSTAMP;VALUE=DATE-TIME:20240704T115536Z
UID:indico-contribution-7-43@meetings.aip.de
DESCRIPTION:Speakers: Shu-ichiro Inutsuka (Nagoya University)\nI try to ex
 plain the primordial origin of misalignment between the disk rotation and 
 host star’s rotation from the context of the disk formation. Theoretical
  and observational investigations have provided convincing evidence for th
 e formation of molecular cloud cores by the gravitational fragmentation of
  filamentary molecular clouds\, which has important implication for the or
 igin of the stellar initial mass function. On the other hand\, the size an
 d total angular momentum of a protoplanetary disk are supposed to be direc
 tly related to the rotational property of the parental molecular cloud cor
 e where the central protostar and surrounding disk are born. Our recent an
 alysis concludes that both the mass function and angular momentum distribu
 tion of molecular cloud core are the natural outcome of transonic turbulen
 ce with Kolmogorov spectrum in parental filamentary molecular clouds. The 
 implication of this identification is non-homogeneous angular momentum dis
 tribution inside a molecular cloud core. The actual angular momentum accre
 tion onto a young stellar object in the core should create misalignment of
  disk surrounding the star. We show the probability distribution of the mi
 salignment as a function of disk mass. This finding may explain the origin
  of misaligned planets created in those disks.\n\nhttps://meetings.aip.de/
 event/1/contributions/43/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/43/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Kinematic signatures of planet-induced warps
DTSTART;VALUE=DATE-TIME:20200515T072500Z
DTEND;VALUE=DATE-TIME:20200515T074500Z
DTSTAMP;VALUE=DATE-TIME:20240704T115536Z
UID:indico-contribution-7-36@meetings.aip.de
DESCRIPTION:Speakers: Alison Young (University of Leicester)\nObservations
  of structures in discs such as gaps and kinks give us a tantalising glimp
 se of possible planets forming there. Recent numerical simulations show th
 at planets that are misaligned with respect to the protoplanetary disc may
  cause the disc to warp and even break into distinct planes. These effects
  occur even with small misalignments and are therefore likely to be reason
 ably common. We have performed chemical models of a disc warped by a plane
 t and used this to predict the kinematic signatures of planet-induced warp
 s. We highlight the most useful diagnostics\, and discuss how observations
  can indicate the presence of a planet at various radii within a protoplan
 etary disc.\n\nhttps://meetings.aip.de/event/1/contributions/36/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/36/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Ring/gaps formation driven by MHD winds in protoplanetary discs
DTSTART;VALUE=DATE-TIME:20200515T070000Z
DTEND;VALUE=DATE-TIME:20200515T072000Z
DTSTAMP;VALUE=DATE-TIME:20240704T115536Z
UID:indico-contribution-7-23@meetings.aip.de
DESCRIPTION:Speakers: Antoine Riols (IPAG Grenoble)\nRings and gaps have b
 een observed in a wide range of proto-planetary discs\, from young systems
  like HLTau to older discs like TW Hydra. Recent disc simulations have sho
 wn that magnetohydrodynamic (MHD) turbulence (in both the ideal or non-ide
 al regime) can lead to the formation of rings and be an alternative to the
  embedded planets scenario. In this talk\, I will investigate the way in w
 hich these ring form in this context and seek a generic formation process\
 , taking into account the various dissipative regimes and magnetisations p
 robed by the past simulations. I will show that a linear instability\, dri
 ven by MHD winds\, might occur and spontaneously form these rings/gaps str
 uctures. Given its robustness\, the process identified could have importan
 t implications for a wide range of accreting systems threaded by large-sca
 le magnetic fields. To make connection with observations\, I will finally 
 analyze the dust distribution around rings/gaps structures and characteriz
 e its emission.\n\nhttps://meetings.aip.de/event/1/contributions/23/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/23/
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