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This study investigates how proto-neutron stars with quark matter cores evolve through different temperature stages by developing hot hybrid equations of state. The researchers used Skyrme effective interactions for hadronic matter and the MIT bag model for quark matter, applying different charge conservation scenarios (Maxwell and Gibbs constructions) to model phases before and after neutrino diffusion. They found that the early evolutionary stages of hybrid stars significantly influence their maximum possible gravitational mass in later stages, regardless of whether electric charge is conserved locally or globally.
Why it matters
Understanding the internal structure and evolution of proto-neutron stars is crucial for interpreting multi-messenger astronomical observations, including gravitational waves and neutrino detection from neutron star mergers and supernovae. These findings help constrain the behavior of matter at extreme densities and temperatures that cannot be replicated in terrestrial laboratories.
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⚠️ Preprint – Noch nicht peer-reviewed
Dieser Artikel wurde noch nicht von unabhängigen Experten begutachtet. Die Ergebnisse sind vorläufig und sollten mit Vorsicht interpretiert werden.
Abstract: The new era of multi-messenger astronomy requires the accurate and self-consistent derivation of the nuclear equation of state at high temperature. In the present work, we focused on the calculation of hot hybrid equations of state, studying the different evolution stages of a proto-neutron star with a quark matter core (proto-hybrid star). For the hadronic matter we used two distinct Skyrme effective interactions, while for quark matter the well-known vector MIT bag model was employed. To model the era of trapped neutrinos in the system we considered the global conservation of lepton fraction which resulted in an equation of state with an extended mixed phase. For periods following the neutrino diffusion phase of a proto-neutron star, the equations of state were modelled using both the Maxwell and the Gibbs construction depending on the assumption for either local or global electric-charge conservation. With the use of the derived hybrid models, we solved the Tolman-Oppenheimer-Volkov equations to describe the corresponding hybrid star configurations. Finally, we investigated how the structure of proto-hybrid stars evolves, using constant rest mass sequences. We found that regardless of whether electric-charge is globally or locally conserved, the earlier stages of a hybrid star’s life may play a crucial role on the determination of its maximum possible gravitational mass in later stages.
Source: Hadron-quark phase transitions along proto-neutron-star evolution