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Impact of Hot Inner Crust on The Properties of Hot Compact Stars

Clara DehmanMario CentellesXavier Vi\~nas
Jan 2024
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摘要原文
We have conducted a study on the thermal properties of the recently developed nuclear energy density functional known as BCPM. This functional is founded on microscopic calculations that incorporate the realistic Argonne $v_{18}$ potential along with Urbana-type three-body forces. BCPM has demonstrated success in describing finite nuclei and cold neutron stars. However, investigating the properties of hot $\beta$-stable matter under both neutrino-free and neutrino-trapped scenarios is vital for astrophysical applications. In this study, we investigate the BCPM equation of state for $\beta$-stable, neutrino-free matter at finite temperatures, taking into consideration the hot inner crust and applying the frozen correlation approximation. Such an equation of state holds significant importance for hot compact objects, such as the final result of a binary neutron star merger event. Our exploration has unveiled the presence of cluster regions, persisting up to a temperature of approximately $7.2$ MeV, denoted as the limiting temperature. Beyond this limiting temperature, clusters are not anticipated to manifest. At temperatures below the limiting threshold, clusters within the inner crust are encompassed by uniform matter with varying densities, facilitating the distinction between the higher and lower transition density branches. Furthermore, we have computed mass-radius relationship, while assuming an isothermal profile for neutron star matter at diverse temperature values. Our findings indicate that the results of the hot inner crust substantially influences the mass-radius relationship, resulting in the formation of larger, more inflated neutron stars. A thorough analysis of the hot inner crust is therefore essential for the study of proto-neutron stars.
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