In this talk I shall review analytical and numerical results on equilibrium configurations of rotating fluid bodies within Einstein's theory of gravitation.
Current numerical relativity codes model neutron star matter as a perfect fluid, with an unphysical "atmosphere" surrounding the star to avoid the breakdown of the equations at the fluid-vacuum interface at the surface of the star. To design numerical methods that do not require an unphysical atmosphere, it is useful to know what a generic sound wave looks near the surface. After a review of relevant mathematical methods, I will present results for low (finite) amplitude waves that remain smooth and, perhaps, for high amplitude waves that form a shock.
The phase transition is a phenomenon that appears in natural sciences in various contexts. In the random graph theory, the phase transition refers to a dramatic change in the number of vertices in the largest components by addition of a few edges around a critical value, which was first discussed on the standard random graphs in the seminal paper by Erdos and Renyi. Since then, the phase transition has been a central theme of the random graph theory. In this talk we discuss the phase transition in random graphs with a given degree sequence and random graph processes with degree constraints.