SSMD Theory II: Proto-Sun Origin by raghav shukla

We extend the Shukla Solar Magneto-Disk Theory (SSMD-II) to provide a quantitative framework for the origin and distribution of angular momentum in the proto-Solar System. While the Classical Nebular Hypothesis (CNH) explains nebular collapse and disk formation, it does not address the mechanisms driving disk rotation.
In SSMD-II, convection within the proto-Sun generates plasma currents that produce seed magnetic fields. These fields dynamically couple with the ionized nebula, exert Lorentz torques, and spin up the disk on timescales shorter than classical viscous models. Seed-field amplification via the α–Ω dynamo is supported by analytical models and 3D MHD simulations.
Theoretical support for the role of magnetic fields is provided by NASA studies (Stepinski& Reyes-Ruiz 1993; DocID: 19940016318), which show that MHD dynamo-generated fields can significantly influence angular momentum and disk structure. Observations from ALMA, SDO/HMI, JWST, SKA, and Aditya-L1 are broadly consistent with SSMD-II predictions. Together, SSMD-II and CNH provide a complementary framework for understanding early Solar System formation.
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