arXiv subjects
Publications and source records attributed to E. Chubarian.
The model and algorithm for the cooling of the magnetized neutron stars are presented. The cooling evolution described by system of parabolic partial differential equations with non-linear coefficients is solved using Alternating Direction Implicit method. The difference scheme and the preliminary results of simulations are presented.
Using the formalism of general relativity for axially symmetric gravitational fields and their sources - rotating compact stars - a perturbation theory with respect to angular velocity is developed and physical quantities such as mass, shape, momentum of inertia and total energy of the star are defined. The change of the internal structure of the star due to rotation has been investigated and the different contributions to the moment of inertia have been evaluated separately. Numerical solutions have been performed using a two-flavor model equation of state describing the deconfinement phase transition as constrained by the conservation of total baryon number and electric charge. During the spin down evolution of the rotating neutron star, below critical values of angular velocity a quark matter core can appear which might be detected as a characteristic signal in the pulsar timing. Within the spin-down scenario due to magnetic dipole radiation it is shown that the deviation of the braking index from $n=3$ could signal not only the occurrence but also the size of a quark core in the pulsar. A new scenario is proposed where, due to mass accretion onto the rapidly rotating compact star, a spin-down to spin-up transition might signal a deconfinement transition in its interior.
The occurence of a quark matter core in rotating compact stars has been investigated within general relativity as a function of both the rotational frequency and the total baryon number. We demonstrate that the deviation of the braking index from $n=3$ signals not only the occurence but also the size of a quark matter core in a pulsar. We suggest that in systems with mass accretion onto a rapidly rotating compact star a spin-down to spin-up transition might signal a deconfinement transition in its interior.