A new temperature dependent hyperonic equation of state: application to rotating neutron star models and I-Q-relations

Understand

In this work we present a newly constructed equation of state (EoS) --applicable to stellar core collapse and neutron star mergers--, including the entire baryon octet.

• Our EoS is compatible with the main constraints from nuclear physics and, in particular, with a maximum mass for cold beta-equilibrated neutron stars of 2 solar masses in agreement with recent observations.
• As an application of our new EoS, we compute numerical stationary models for rapidly (rigidly) rotating hot neutron stars.
• We consider maximum masses of hot stars, such as proto-neutron stars or hypermassive neutron stars in the post-merger phase of binary neutron star coalescence.