Tuesday 24 January 2017, 4.00PM
Speaker(s): Isaac Vidaña Haro
Neutron stars are the remants of the gravitational collapse of massive stars during a Type-II, Ib or Ic supernova explosion. Their masses and radii are typically of the order of 1-2 M_sun and 10-12 km, respectively. With central densities in the range of 4-8 times normal nuclear saturation density, neutron stars are most likely among the densest objects in the Universe. These objects are an excellent observatory to test our present understanding of the theory of strong interacting matter at extreme conditions, and they offer an interesting interplay between nuclear processes and astrophysical observables. Conditions of matter inside neutron stars are very different from those one can find in Earth, therefore, a good knowledge of the equation of state of dense matter is required to understand the properties of neutron stars. Nowadays, it is still an open question which is the true nature of neutron stars. Traditionally the core of neutron stars has been modeled as a uniform fluid of neutron-rich matter inequilibrium with respect to the weak interaction. Nevertheless, due to the large value of the density, new hadronic or even non-hadronic degrees of freedom are expected to appear in addition to nucleons. In this talk I will review some of the properties of these fascinating objects.