Speaker
David Blaschke
(University of Wroclaw)
Description
We introduce two sets of models with symmetry energy functionals which at
high baryon densities differ in stiffness. The symmetric part of the energy
per baryon is the same for all models and is based on the APR EoS. We test
the behavior of the symmetry energy by using a constraint on the total
baryon mass for a gravitational mass of a 1.25 M$_{\odot}$ neutron star.
This constraint is the result of an study perfomed by Kitaura et al. on
stellar explosions of stars with an O-Ne_Mg core. Since the symmetry energy
is closely related to the proton fraction of neutron star matter, we discuss
the role of the DUrca cooling since it can be activated above some threshold
on the proton content. We conclude with showing the favored models and their
corresponding effects on the neutron star radius.
Author
Co-author
David Blaschke
(University of Wroclaw)
