http://arxiv.org/abs/1907.13375
Neutron stars are among the densest known objects in the universe and an ideal laboratory for the strange physics of super-condensed matter. While the simultaneously measurement of mass and radius of non-rotating neutron stars may impose strong constraints on the properties of the dense nuclear matter, the observation and study of rapidly-rotating ones, close to the mass-shedding limit, may lead to significantly further constraints. Theoretical predictions allow neutron stars to rotate extremely fast (even more than $2000 \ {\rm Hz}$). However, until this moment, the fastest observed rotating pulsar has a frequency of $716 \ {\rm Hz}$, much lower compared to the theoretical predictions. There are many suggestions for the mechanism that leads to this situation. In any case, the theoretical study of uniformly rotating neutron stars, along with the accurate measurements, may offer rich information concerning the constraints on the high density part of the equation of state. In addition, neutron stars through their evolution, may provide us with a criteria to determine the final fate of a rotating compact star. Sensitivity of bulk neutron stars properties on the equation of state at the mass-shedding limit, are the main subject of the present study.
P. Koliogiannis and C. Moustakidis
Thu, 1 Aug 19
36/66
Comments: 16 pages, 24 figures
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