Seminarium: On the neutron stars modeling
- Datum: –15.00
- Plats: Ångströmlaboratoriet Hjorter’s room (Å73101)
- Föreläsare: Giovanni Camelio, Stockholms Universitet
- Kontaktperson: Sofia Ramstedt
Neutron stars are one of the possible results of supernova explosions and of binary neutrons star mergers. Due to their compactness, neutron stars have at the same time a very large gravitational field and extreme matter densities, features that make them interesting both to astrophysicists and nuclear physicists. In the first part of this talk I will discuss how a simple model of rotating neutron stars allows us to rule out a possible channel of short gamma ray burst emission. We accomplished this by studying the stability of a rigidly rotating, cold neutron star and estimating the amount of mass that would escape black hole formation.
In the second part of this talk I will present a new technique to model the stationary configuration of hot, rotating neutron stars that for the first time does not require barotropicity, that is, that the pressure is in a one-to-one relation with the other thermodynamic quantities.This is important because a newly formed neutron star is in no way barotropic, and its better modeling will improve the observational predictions. Our method to obtain non-barotropic configurations is novel even in the context of Newtonian stars, to whom it can be easily applied.
Tim Dietrich, Miguel Marques, Stephan Rosswog