2021/05/16 by Enping Zhou, Kenta Kiuchi, Masaru Shibata +3 · 13 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Bottom quark #Differential rotation #Exotic star #Gamma-ray bursts and supernovae #Gravitational wave #Neutron star #Particle physics #Physics #Pulsars and Gravitational Waves Research #Quark #Quark star #Stars #Strange matter #Top quark #Top quark condensate #Up quark #astro-ph.HE #gr-qc
paper · pdf · doi:10.1103/physrevd.103.123011
published in Physical review. D/Physical review. D. 103(12) (American Physical Society) · 17 pages, 17 figures; accepted for publication in PRD (submitted to PRD in July 2020)
arxiv created 2021/05/16 · openalex created_date 2021/05/24 · openalex publication_date 2021/06/08 · arxiv updated 2021/06/09 · openalex updated_date 2026/08/06
We introduce our approaches, in particular, the modifications of the primitive recovery procedure, to handle bare quark stars in numerical relativity simulations. Reliability and convergence of our implementation are demonstrated by evolving two triaxially rotating quark star models with different mass as well as a differentially rotating quark star model which has sufficiently large kinetic energy to be dynamically unstable. These simulations allow us to verify that our method is capable of resolving the evolution of the discontinuous surface of quark stars and possible mass ejection from them. The evolution of the triaxial deformation and the properties of the gravitational-wave emission from triaxially rotating quark stars are also studied, together with the mass ejection of the differentially rotating case. We find that supramassive quark stars are not likely to be ideal sources of a continuous gravitational wave as the star recovers axisymmetry much faster than models with smaller mass and gravitational-wave amplitude decays rapidly in a timescale of 10 ms, although the instantaneous amplitude from more massive models is larger. As with the differentially rotating case, our result confirms that quark stars could experience nonaxisymmetric instabilities similar to the neutron star case but with a quite small degree of differential rotation, which is expected according to previous initial-data studies.