2D MRI-induced turbulence in high $\beta$ PIC simulation

The magnetorotational instability (MRI) is a crucial mechanism of angular momentum transport in a variety of astrophysical scenarios, as accretion disks nearness neutron stars and black holes. The MRI has been widely studied using MHD models and simulations, in order to understand the behaviour of astrophysical fluids in a state of differential rotation. When the timescale for electron and ion collisions is longer than the inflow time in the disk, the plasma is macroscopically collisionless and MHD breaks down. This is the case of the limit of weak magnetic field, i.e., as the ratio of the ion cyclotron frequency to orbital frequency becomes small. Leveraging on the recent addition of the shearing co-rotating frames equations of motion and Maxwell's equations modules in our PIC code OSIRIS 3.0, we intend to present our recent results of the analysis of MRI in collisionless plasma. Increasing the scale of our simulations, we will show the first ab-initio PIC simulations of a 2D turbulence induced consistently during the saturation regime of the MRI. We will demonstrate the existence of a minimum scale $\lambda_{kink}$ that determine the comparison of a drift-kink instability in the plasma. This instability will activate the turbulence during the saturation regime of the MRI.