Exploring complexity in the presence of shear and heat dissipation

Abstract We analyze the complexity factor in spherically symmetric stars undergoing dissipative collapse in the presence of shear. The interior spacetime is described by a general spherically symmetric metric, and the corresponding Einstein field equations are derived. Matching the interior spacetime to the exterior Vaidya geometry yields the boundary condition governing the temporal evolution of the collapsing body. The interior matter distribution obeys the Euclidean condition, i.e. the areal radius is identical to the proper radius as the star collapses. We present a complete model of a Euclidean star and investigate its physical viability. We further investigate the notion of complexity as defined by Herrera in terms of the pressure anisotropy, density inhomogeneity and heat flux. The novelty of our work is the demonstration of the interplay of these factors to the complexity in a shearing model which is absent in earlier treatments.