Massive Star Formation through Direct Collapse regulated by the Magnetic Field

Recent simulations of massive star formation reveal that high mass accretion rates can prevent the formation of an intermediate hydrostatic "first core" (1-10 AU). Leading to a continuous, supersonic infall of matter directly onto the forming star, and bypassing the disk formation typically observed in low-mass star formation. In the absence of the first core, magnetic field dissipation is minimized, enabling magnetic braking to remain highly effective throughout the collapse. This results in a different evolutionary pathway for massive stars, characterized bydirect accretion onto the proto-star, weak outflows, and the absence of a rotationally supported disk (Dapp et al., 2012; Tsukamoto et al., 2015). These observations deviate from traditional star formation models, necessitating a re-evaluation of the role of magnetic fields and mass accretion dynamics in the formation of massive stars