Brown Dwarf Formation Through Gravitational Collapse: Insights From 3D Numerical Simulations

The formation mechanism of Brown Dwarfs (BDs), whether akin to stars or ejected planetary-mass objects, remains debated. We present the first 3D radiation-MHD simulations of magnetized, turbulent, gravitationally unstable low-mass cores ($0.05-0.1{\mathrm{M}}_{\odot }$) collapsing into proto-BDs. Using the {\ttfamily RAMSES} code with adaptive mesh refinement, we model the full dynamical range (${10}^5-{10}^{22}\mathrm{c}{\mathrm{m}}^{-3}$), including radiative transfer (flux limited diffusion) and non-ideal MHD (ambipolar diffusion). Our simulations self-consistently follow the isothermal collapse, first hydrostatic core formation, H${}_2$ dissociation, and BD birth. The resulting BDs have initial radii $\approx 0.75{\mathrm{R}}_{\odot }$ and masses $\approx 0.8{\mathrm{M}}_{\mathrm{J}\mathrm{u}\mathrm{p}}$, growing via accretion as we follow the early evolution of the object. Crucially, we find that BDs may form similarly to low-mass stars but with a prolonged first-core phase, supporting a star-like formation scenario.