Speaker
Description
Matter inside neutron stars and their mergers can reach densities of more than 10 times normal nuclear density. In such extreme environments, new particles and phases of matter appear, as well as different interactions become important. In my lectures, I review old and new ways to use neutron star observables to learn about dense matter, comment on what we know and what we expect to discover within the next years concerning dense matter, and provide an overview of modern ways to build and share dense matter descriptions (usually referred to as equations of state).
Modelling dense matter:
1) Speed of sound of dense matter
2) Example of parametric approach
3) RMF models (beyond Walecka covered by Andreas)
4) Chiral models
5) Dense matter EoS repositories