Counter-Rotating Fluid Dynamics in a Riemann-Cartan Spacetime: Kinetic Theory, Boltzmann Transport, and Geometric Thermalization within the Seashell-Universe Model

We extend the theoretical framework of the Field Dynamics Conjecture within the static conoidalhelicoidal geometry of the Seashell-Universe Model by introducing the formal mechanics of counterrotatingfluid fields. While the baseline metric structure relies on a quadratic angular line elementindependent of the directional sign of the helical trajectory, the micro-physical implications ofco-existing clockwise (θ˙ < 0) and counter-clockwise (θ˙ > 0) particle currents have remained unaddressed.In this paper, we derive the exact step-by-step mathematical foundations of relativisticBoltzmann transport for counter-rotating plasma domains under asymmetric affine connections.We demonstrate that the microscopic scattering and frontal collisions of these opposing currentsprovide the precise, first-principles physical mechanism driving the stochastic averaging of the backgroundcontorsion tensor into the macroscopic geometric damping coefficient Ktorsion. Furthermore,we analyze the thermodynamic impact of these collisions within the ultra-dense quantum bounceregime near the conoidal vertex (¯R → 1.0), where the dynamic suppression of the Higgs vacuumexpectation value renders all fundamental fermions massless. This complete absence of inertial masseliminates gravitational clustering instabilities and transforms frontal counter-rotating impacts intoa highly efficient, unresisted causal thermalization engine, offering a parsimonious resolution to thecosmological horizon paradox without cosmic inflation.