Speaker
Description
Rings and gaps have been observed in a wide range of proto-planetary discs, from young systems like HLTau to older discs like TW Hydra. Recent disc simulations have shown that magnetohydrodynamic (MHD) turbulence (in both the ideal or non-ideal 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 which these ring form in this context and seek a generic formation process, taking into account the various dissipative regimes and magnetisations probed by the past simulations. I will show that a linear instability, driven by MHD winds, might occur and spontaneously form these rings/gaps structures. Given its robustness, the process identified could have important implications for a wide range of accreting systems threaded by large-scale magnetic fields. To make connection with observations, I will finally analyze the dust distribution around rings/gaps structures and characterize its emission.
