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Stars form from the gravitational collapse of turbulent, magnetized molecularcloud cores. Our non-ideal MHD simulations reveal that the intrinsicallyanisotropic magnetic resistance to gravity during the core collapse naturallygenerates dense gravo-magneto-sheetlets within inner protostellar envelopes --disrupted versions of classical sheet-like pseudodisks. They are embedded in amagnetically dominant background, where less dense materials flow along thelocal magnetic field lines and accumulate in the dense sheetlets. Thesheetlets, which feed the disk predominantly through its upper and lowersurfaces, are the primary channels for mass and angular momentum transfer fromthe envelope to the disk. The protostellar disk inherits a small fraction (upto 10\%) of the magnetic flux from the envelope, resulting in a disk-averagednet vertical field strength of 1-10 mG and a somewhat stronger toroidal field,potentially detectable through ALMA Zeeman observations. The inherited magneticfield from the envelope plays a dominant role in disk angular momentumevolution, enabling the formation of gravitationally stable disks in caseswhere the disk field is relatively well-coupled to the gas. Its influenceremains significant even in marginally gravitationally unstable disks formed inthe more magnetically diffusive cases, removing angular momentum at a ratecomparable to or greater than that caused by spiral arms. The magneticallydriven disk evolution is consistent with the apparent scarcity of prominentspirals capable of driving rapid accretion in deeply embedded protostellardisks. The dense gravo-magneto-sheetlets observed in our simulations maycorrespond to the ``accretion streamers" increasingly detected aroundprotostars.

Protostellar Disks Fed By Dense Collapsing Gravo-Magneto-Sheetlets