We present a refined phenomenological relation for estimating the critical mass of a neutron star (NS), accounting for both rotation and magnetic helicity effects. This model is analyzed to confirm agreement with recognized universal relations, constrained based on observations from both gravitational wave and electromagnetic sources, and results of surface deformation derived using X-ray pulse modeling add dependencies involving the moment of inertia and compactness. Our model builds on the classical static Tolman–Oppenheimer–Volkoff limit by adding important physical effects: centrifugal pressure from rapid spin combined with magneto-superfluid effects that display magnetic helicity in the NS core and deformation of the stellar surface resulting from high rotational spin rates. The model accurately reproduces key numerical results as seen in the quasi-universal relation  for configurations with maximum rotation. This refined approach leads to a gentle, flexible tool for estimating critical masses and interpreting observational data for rotating systems and magnetized compact stars, where it contributes to ongoing analytical and numerical developments in relativistic astrophysics.

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