Properties of relativistically rotating quark stars

5th Compact Stars in the QCD Phase Diagram

Zhou, Enping^1

Department of Astronomy, Peking University, Beijing

100871, China^1

关键词: Equation of state;    Future observations;    Gravitational radiation;    Gravitational-wave observatory;    Millisecond pulsars;    Numerical relativity;    Polynomial equation;    Strong interaction;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/861/1/012007/pdf
DOI  :  10.1088/1742-6596/861/1/012007

来源: IOP

【 摘 要 】

In this work, quasi-equilibrium models of rapidly rotating triaxially deformed quark stars are computed in general relativistic gravity, assuming a conformally flat spatial geometry (Isenberg-Wilson-Mathews formulation) and a polynomial equation of state. Especially, since we are using a full 3-D numerical relativity initial data code, we are able to consider the triaxially deformed rotating quark stars at very high spins. Such triaxially deformed stars are possible gravitational radiation sources detectable by ground based gravitational wave observatories. Additionally, the bifurcation from axisymmetric rotating sequence to triaxially rotating sequence hints a more realistic spin up limit for rotating compact stars compared with the mass-shedding limit. With future observations such as sub-millisecond pulsars, we could possibly distinguish between equation of states of compact stars, thus better understanding strong interaction in the low energy regime.