Dense matter in neutron stars

Institutskolloquium

  • Datum: 04.05.2018
  • Uhrzeit: 10:30 - 12:00
  • Vortragende(r): Prof. Dr. Jürgen Schaffner-Bielich
  • Universität Frankfurt
  • Ort: Garching und Greifswald
  • Raum: Hörsaal D2 (Übertragung nach HGW S1)
Neutron stars are born as the endpoint of stellar evolution in core-collapse supernovae. The densities in a neutron star are extremely high, so high that nuclei are squeezed into their constituents, neutrons and protons. Exotic matter can appear in the core, either in the form of hyperons or as a new phase in the form of strange quark matter. The properties of neutron stars are determined by the nuclear equation of state of dense matter, so that the observation of neutron stars and neutron star merger can give a telltale signature of the properties of dense matter under extreme conditions. The present astrophysical data on neutron stars and pulsars, rotation-powered neutron stars, is reviewed. The equation of state of dense matter will be discussed and possible implications for future observations of core-collapse supernovae and neutron star mergers will be outlined.
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