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 explore the implications of a strong first-order phase transition regionin the dense matter equation of state in the interiors of rotating neutronstars, and the resulting creation of two disjoint families of neutron-starconfigurations (the so-called high-mass twins). We numerically obtainedrotating, axisymmetric, and stationary stellar configurations in the frameworkof general relativity, and studied their global parameters and stability. Theinstability induced by the equation of state divides stable neutron starconfigurations into two disjoint families: neutron stars (second family) andhybrid stars (third family), with an overlapping region in mass, the high-masstwin-star region. These two regions are divided by an instability strip. Itsexistence has interesting astrophysical consequences for rotating neutronstars. We note that it provides a natural explanation for the rotationalfrequency cutoff in the observed distribution of neutron star spins, and forthe apparent lack of back-bending in pulsar timing. It also straightforwardlyenables a substantial energy release in a mini-collapse to another neutron-starconfiguration (core quake), or to a black hole.

Consequences of a strong phase transition in the dense matter equation of state for the rotational evolution of neutron stars