Stars and their corresponding protoplanetary disks form in diverse environments .
To account for these natural variations , we investigate the formation process around nine solar mass stars with a maximum resolution of 2 AU in a Giant Molecular Cloud of ( 40 pc ) ^ { 3 } in volume by using the adaptive mesh refinement code ramses .
The magnetohydrodynamic simulations reveal that the accretion process is heterogeneous in time , in space , and among protostars of otherwise similar mass .
During the first roughly 100 kyr of a protostar evolving to about a solar mass , the accretion rates peak around 10 ^ { -5 } to 10 ^ { -4 } M _ { \odot } yr ^ { -1 } shortly after its birth , declining with time after that .
The different environments also affect the spatial accretion , and infall of material to the star-disk system is mostly through filaments and sheets .
Furthermore , the formation and evolution of disks varies significantly from star to star .
We interpret the variety in disk formation as a consequence of the differences in the combined effects of magnetic fields and turbulence that may cause differences in the efficiency of magnetic braking , as well as differences in the strength and distribution of specific angular momentum .