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SUMMARY:Hot and thick discs: stability of Initial Conditions and prelimina
 ry results
DTSTART;VALUE=DATE-TIME:20200512T100000Z
DTEND;VALUE=DATE-TIME:20200512T102000Z
DTSTAMP;VALUE=DATE-TIME:20240704T115618Z
UID:indico-contribution-51@meetings.aip.de
DESCRIPTION:Speakers: Marco Cilibrasi (University of Zurich)\nBoth the Cor
 e Accretion and the Gravitational Instability models for giant planet form
 ation predict the presence of circumplanetary discs (CPDs) during the last
  formation phases (Alibert et al. 2005\, Ward & Canup 2010). These discs a
 re found to be continuously fed by an influx of gas from the protoplanetar
 y disc (Tanigawa et al. 2012). Magnetic fields generated by the disc itsel
 f could play a key role in modeling this accretion flow (Gressel et al. 20
 13). In the early stages of a giant planet's life\, the magnetic field gen
 erated by the planet could be even stronger\, thus potentially important d
 epending on how it couples with the surrounding flow (Yadav et al. 2017 an
 d Cauley et al. 2019)\, and possibly dominant.\nIn the Core Accretion scen
 ario\, CPDs are expected to be very hot and thick when forming. For such d
 iscs\, regardless of their nature (CPD or PPD)\, standard thin-disc approx
 imations can not be used to set ICs and new numerical and analytical metho
 ds have to be investigated\, to ensure especially equilibrium at boundarie
 s. Here we present a study of equilibrium initial conditions for thick and
  hot disc simulations with the meshless finite mass (MFM) method in the GI
 ZMO code (Hopkins 2015\; Deng et al.2019)\, which can be used by any code 
 utilizing a particle-based representation of the fluid. \nTime permitting
 \, we will show preliminary results obtained after setting a CPD initial c
 ondition with these methods and adding magnetic fields to our simulation.\
 n\nhttps://meetings.aip.de/event/1/contributions/51/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/51/
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