English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We study the thermal evolution of neutron stars described within the equationof state with induced surface tension (IST) that reproduces properties ofnormal nuclear matter, fulfills the proton flow constraint, provides ahigh-quality description of hadron multiplicities created during thenuclear-nuclear collision experiments, and it is equally compatible with theconstraints from astrophysical observations and the GW170817 event. The modelfeatures strong direct Urca processes for the stars above $1.91~M_{\odot}$. TheIST equation of state shows very good agreement with the available coolingdata, even without introducing nuclear pairing. We also analysed the effect ofthe singlet proton/neutron and triplet neutron pairing on the cooling ofneutron stars of different mass. We show that the description of the compactobject in the center of the Cassiopeia A does not necessarily require aninclusion of neutron superfluidity and/or proton superconductivity. Our resultsindicate that data of Cassiopeia A can be adequately well reproduced by a$1.66~M_{\odot}$ star with an atmosphere of light elements. Moreover, the ISTEoS reproduces each of the observational datasets for the surface temperatureof Cassiopeia A either by a rapidly cooling $\sim$ $1.955~M_{\odot}$ star withpaired and unpaired matter or by a $1.91~M_{\odot}$ star with the inclusion ofneutron and proton pairings in the singlet channel.

Neutron star cooling within the equation of state with induced surface tension