Speaker
Hannes Rüter
(CENTRA, Departamento de Física, Instituto Superior Técnico, Universidade de Lisboa)
Description
Relativistic stars are typically modelled as ideal fluids. In this talk I discuss the numerical construction of solutions for spherical, relativistic stars at finite temperature within full kinetic theory. In this case matter is described by the Vlasov-Boltzmann equation, which allows for a more realistic description of stars that is valid beyond the hydrodynamic limit. I discuss the new physical effects occuring in this model and compare with the ideal fluid stars given by the Tolman-Oppenheimer-Volkoff solution.
Author
Hannes Rüter
(CENTRA, Departamento de Física, Instituto Superior Técnico, Universidade de Lisboa)
