Speaker
Description
Both the Core Accretion and the Gravitational Instability models for giant planet formation predict the presence of circumplanetary discs (CPDs) during the last formation phases (Alibert et al. 2005, Ward & Canup 2010). These discs are found to be continuously fed by an influx of gas from the protoplanetary disc (Tanigawa et al. 2012). Magnetic fields generated by the disc itself could play a key role in modeling this accretion flow (Gressel et al. 2013). In the early stages of a giant planet's life, the magnetic field generated by the planet could be even stronger, thus potentially important depending on how it couples with the surrounding flow (Yadav et al. 2017 and Cauley et al. 2019), and possibly dominant.
In the Core Accretion scenario, CPDs are expected to be very hot and thick when forming. For such discs, regardless of their nature (CPD or PPD), standard thin-disc approximations can not be used to set ICs and new numerical and analytical methods have to be investigated, to ensure especially equilibrium at boundaries. Here we present a study of equilibrium initial conditions for thick and hot disc simulations with the meshless finite mass (MFM) method in the GIZMO code (Hopkins 2015; Deng et al.2019), which can be used by any code utilizing a particle-based representation of the fluid.
Time permitting, we will show preliminary results obtained after setting a CPD initial condition with these methods and adding magnetic fields to our simulation.
