Later chapters address well-posedness questions for the classical Skyrme model
, equivariant wave maps, and the phenomenon of collapse for wave maps.
where a(t) is the acceleration of the particle; R(t) is the radial distance of the particle or simply the radius of the neutron star; [rho](R) is the density of neutron star; P([rho]) is the pressure of neutron star, which in this study is given by the Skyrme model
for the Equation of State (EOS) of neutron stars [21,22],
Among the topics are skyrmions and nuclei, rotational symmetry breaking in baby Skyrme models
, noncommutative skyrmions in quantum Hall ferromagnets, half-skyrmion theory for high-temperature superconductivity, holographic baryons, and baryon physics in a five-dimensional model of hadrons.