Final Activity Report Summary - DYNEOS (Constraints for the realistic equation of state of dense matter from the dynamical evolution of compact star space-times)
The project was intrinsically multidisciplinary and necessarily demanded to combine the knowledge from many different fields of physics of different scales (macro- and micro-physics), especially the General Theory of Relativity and the modern theory of dense matter (quantum mechanics, thermodynamics, nuclear physics...) astrophysics as well as applied mathematics (numerical algorithms) and advanced programming in order to use and develop numerical methods for solving multi-dimensional computational problems than cannot be solved analytically. The multidisciplinary treatment provided natural balance between analytical considerations and numerical calculations and was intrinsically connected with the choice of problems considered.
The ultimate goal was to explore the mysterious and presently at large unknown interiors of compact astrophysical objects, thus studying the properties of extremely dense matter that is not likely to be accomplished in Earth-based experiments in near future. Proposed calculations aimed into precise numerical simulations of dynamics of compact objects within the framework of General Relativity. The use of certain verified in practice numerical techniques, namely pseudo-spectral methods, combined if neccesary with finite-differences methods, provided desired flexibility for optimal results.
Developed state-of-the artnumerical codes gave opportunity for studying wide range of interesting unsolved problems, such as the state of rapidly rotating compact stars, oscillation and stability of non-linear modes for rotating stars, dynamical re-configuration of the star structure induced by the appearance of exotic phase core (so-called mini-collapse), inclusion of various realistic processes (i.e. accretion, viscosity, magnetic fields), elastic properties of the crust of spinning-down pulsars as well as direct computation of resulting gravitational wave emission in various physical settings.
The ultimate goal was to explore the mysterious and presently at large unknown interiors of compact astrophysical objects, thus studying the properties of extremely dense matter that is not likely to be accomplished in Earth-based experiments in near future. Proposed calculations aimed into precise numerical simulations of dynamics of compact objects within the framework of General Relativity. The use of certain verified in practice numerical techniques, namely pseudo-spectral methods, combined if neccesary with finite-differences methods, provided desired flexibility for optimal results.
Developed state-of-the artnumerical codes gave opportunity for studying wide range of interesting unsolved problems, such as the state of rapidly rotating compact stars, oscillation and stability of non-linear modes for rotating stars, dynamical re-configuration of the star structure induced by the appearance of exotic phase core (so-called mini-collapse), inclusion of various realistic processes (i.e. accretion, viscosity, magnetic fields), elastic properties of the crust of spinning-down pulsars as well as direct computation of resulting gravitational wave emission in various physical settings.