The Kawasaki model is not exactly solvable as any choice of the exchange rate (w jj ′ ) which satisfies the detailed balance condition is highly nonlinear. In this work we address the issue of writing w jj ′ in a best possible linear form such that the mean squared error in satisfying the detailed balance condition is least. In the continuum limit, our approach leads to a Cahn-Hilliard equation of conservative dynamics. The work presented in this paper will help us anticipate how the conservative dynamics of an arbitrary Ising system depends on the temperature and the coupling constants. In particular, for two and three dimensional systems, the critical temperatures estimated in our work are in good agreement with the actual values. We also calculate the dynamic and some of the critical exponents of the model.

We show Zeeman-like splitting in the energy of spinors propagating in a background gravitational field, analogous to the spinors in an electromagnetic field, otherwise termed the Gravitational Zeeman Effect. These spinors are also found to acquire a geometric phase, in a similar way as they do in the presence of magnetic fields. However, in a gravitational background, the Aharonov-Bohm type effect, in addition to Berry-like phase, arises. Based on this result, we investigate geometric phases acquired by neutrinos propagating in a strong gravitational field. We also explore entanglement of neutrino states due to gravity, which could induce neutrino-antineutrino oscillation in the first place. We show that entangled states also acquire geometric phases which are determined by the relative strength between gravitational field and neutrino masses.

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We show that spinors propagating in curved gravitational background acquire an interaction with spacetime curvature, which leads to a quantum mechanical geometric effect. This is similar to what happens in the case of magnetic fields, known as Pancharatnam-Berry phase. As the magnetic and gravitational fields have certain similar properties, e.g. both contribute to curvature, this result is not difficult to understand. Interestingly, while spacetime around a rotating black hole offers Aharonov-Bohm and Pancharatnam-Berry both kinds of geometric effect, a static spacetime offers only the latter. In the bath of primordial black holes, such gravity induced effects could easily be measured due to their smaller radius.