Nowadays it is well accepted that present-day stars form almost exclusively in the filamentary structures that pervade molecular clouds, being the intersection of massive filaments, known as hub filament systems (HFS), the preferential sites for high-mass star formation.
Observationally, hub filament systems are characterized as the intersection of several massive filaments, in a planar distribution organized radially around a central density enhancement, with typical sizes ranging from a few parsecs to a few tens of parsecs wide. Even though filamentary structures have been observationally and theoretically studied, HFS remain relatively unexplored, and key features, such as the gas kinematics and magnetic field structure, are still a matter of debate.
We present ideal MHD simulations aiming to explore the formation of flat and radially concentrated hub-like structures, as well as the evolution of the gas distribution and kinematics in the HFS.
We find that turbulence plays an essential role in delaying the collapse, allowing the development of filamentary structures that will organize in flattened radial structures through a combination of magnetic pressure, shocks, and gravity.