Adaptive-mesh MHD simulations of a jet emerging from a circumplanetary disc embedded in a protosolar nebula

We perform magnetohydrodynamic computer simulations of a semi-global protoplanetary disc section with an embedded planet core. The disc model assumes a self-consistent and dynamically evolving Ohmic resistivity, which is derived from a sophisticated ionisation model [5, 9] resulting in a dead-zone comparable to our previous local shearing box models [4]. Before the insertion of the planet core, the resulting configuration consists of a magnetically inactive dead zone and turbulent surface layers. When the embedded planet core of initially 100 earth masses has opened a gap in the disc, we study the ionisation structure and turbulent state of this region, including the circumplanetary disc which has formed around the planet. By determining accretion rates and analysing the flow structure in the vicinity of the planet, we aim to address the important question of what limits the growth of gas giant planets in the classic core-accretion picture.