Summary
This project corresponds to a series of 3 papers.
We used state-of-the-art three-dimensional adaptive-mesh-refinement models of massive dense core collapse, which integrate the equations of (resistive) grey radiation magnetohydrodynamics, and include sink particle evolution. For the first time, we include both protostellar radiative feedback via pre-main-sequence evolutionary tracks and magnetic ambipolar diffusion.
The adaptive mesh refinement scheme is employed to resolve scales up to about ~5 AU.
In the first paper (Commerçon et al. A&A 2022, 658:A52 - Paper I), we focus on the role of magnetic fields and ambipolar diffusion in the formation of outflows and discs. We studied three different cases: a purely hydrodynamical run, a magnetised simulation under the ideal approximation (perfect coupling), and a calculation with ambipolar diffusion (resistive case). In the most micro-physically complex model (resistive MHD), we also investigated the effect the initial amplitude of both magnetic field and solid body rotation have on the final properties of the massive protostellar system.
In the next two papers (Mignon-Risse et al. A&A 2021, 652:A69, and Mignon-Risse et al. A&A 2021, 656:A85 - Papers II and III), we stick to the non-ideal MHD setup but we set an initial turbulence field within the cloud and include a hybrid radiative transfer method for stellar irradiation. We varied the Mach and Alfvénic Mach numbers to probe sub- and super-Alfvénic turbulence and sub- and supersonic turbulence regimes.
