Evolution of bare quark stars in full general relativity: Single star case
Authors: Enping Zhou, Kenta Kiuchi, Masaru Shibata, Antonios Tsokaros, Koji Uryu
Abstract
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 have been also studied, together with the mass ejection of the differentially rotating case. It is found that supramassive quark stars are not likely to be ideal sources of 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 non-axisymmetric instabilities similar to the neutron star case but with quite small degree of differential rotation, which is expected according to previous initial data studies.
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Fully general-relativistic simulations of isolated and binary strange quark starsZhenyu Zhu, Luciano Rezzolla · 2021 · High Energy Astrophysical Phenomena · cited 9 times · AI summary available
Abstract
The hypothesis that strange quark matter is the true ground state of matter has been investigated for almost four decades, but only a few works have explored the dynamics of binary systems of quark stars. This is partly due to the numerical challenges that need to be faced when modelling the large discontinuities at the surface of these stars. We here present a novel technique in which the EOS of a quark star is suitably rescaled to produce a smooth change of the specific enthalpy across a very thin crust. The introduction of the crust has been carefully tested by considering the oscillation properties of isolated quark stars, showing that the response of the simulated quark stars matches ac…
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Abstract
Quark stars — hypothetical compact stars made entirely of deconfined quark matter — offer a clean testing ground for gravity beyond general relativity. We study their structure in f(T, Τ ) gravity, a teleparallel theory in which torsion is coupled directly to the trace of the energy--momentum tensor through a single constant coupling. Using the standard MIT bag description of quark matter, we solve the modified stellar structure equations and follow how the mass, radius, compactness, and surface redshift respond as the coupling is varied across its full admissible range. The maximum mass turns out to depend on the coupling in a non-monotonic way: it rises above the general relativity value, …
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Abstract
In a previous work, we explored the possibility of neutron stars with large quark cores. Through Bayesian inference, we obtained large sets of equations of state imposing constraints regarding the properties of nuclear matter, mass-radius data from NICER, the GW170817 data from Virgo-LIGO collaboration, perturbative QCD and causality. We also imposed that the maximum mass neutron star (NS$\text{max}$) must have a large quark core. In this work, we obtain a new set of equations of state (SmallQ set) with the same constraints as before. However, we relaxed the last constraint, imposing only that NS$\text{max}$ must have quark core, regardless of its size. We compare the results with the set fr…
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Abstract
Universal, equation-of-state (EOS) insensitive relations among the global properties of compact stars are well established for hadronic neutron stars and for self-bound strange stars. We ask whether analogous relations hold for the quark core of a hybrid star, and whether the core can be constrained from the surface. Describing quark matter with the three-flavor MIT bag model with repulsive vector interactions, matched to the hadronic DD2 EOS through a Maxwell construction, we scan the full $(B^{1/4},G_V)$ plane and obtain 1112 hybrid EOSs with maximum masses above $2\,M_\odot$, broadly compatible with current multimessenger constraints. For every stable configuration we evaluate the mass, r…
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Abstract
We investigate the hydrostatic equilibrium and global structure of neutron stars within symmetric teleparallel gravity, where gravitational interactions are mediated by the non-metricity scalar $Q$. Working within the metric-affine formulation, we adopt the regular, constant-$Q$ branch ($Q = Q_*$) of $f(Q)$ gravity, which preserves regularity at the stellar centre while maintaining explicit dependence on the non-linear functional form through $f(Q_*)$ and its derivatives. We propose three novel non-linear $f(Q)$ extensions: (i) a Born-Infeld-inspired model, (ii) a Hu--Sawicki analogue, and (iii) a Tsujikawa-inspired model. Incorporating state-of-the-art realistic unified equations of state, …
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This study simulates bar-mode instability in differentially rotating neutron stars, a related compact-star instability to the non-axisymmetric instability examined in quark stars.
Abstract
We investigate the effects ultralight bosonic field dark matter may have on the dynamics of unstable differentially-rotating neutron stars prone to the bar-mode instability. To this aim we perform numerical simulations in general relativity of rotating neutron stars accreting an initial spherically symmetric bosonic field cloud, solving the Einstein-(complex, massive) Klein-Gordon-Euler and the Einstein-(complex) Proca-Euler systems. We find that the presence of the bosonic field can critically modify the development of the bar-mode instability of neutron stars, depending on the total mass of the bosonic field and on the boson particle mass. In some cases, the accreting bosonic field can eve…
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Abstract
This paper investigates a semi-relativistic model describing self-gravitating boson stars. The model is derived from the semi-relativistic Hartree equation with Newtonian gravitational potential, where the kinetic energy is represented by the operator $\sqrt{-\Delta + m^2}$. It is well known that such systems possess a critical mass, analogous to the Chandrasekhar limit for fermion stars. Our main objective is to analyze the asymptotic behavior and the mass concentration mechanism near this critical regime. These results shed light on the mathematical nature of self-gravitational collapse in bosonic systems and extend existing nonrelativistic theories to the semi-relativistic framework. In p…
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Adiabatic evolution of hadronic neutron starsD. Logoteta, Francesco Zeno Constanzo, I. Bombaci et al. · 2026 · Not summarized yet
Abstract
In this paper we compute several structural properties of static and rotating neutron stars, considering both rigid and differential rotation. To this end, we use a finite-temperature beta-stable equation of state (EOS) extending the zero-temperature hadronic EOS derived by Fortin et al. (2017). We account for the formation of hyperons and the presence of a neutrino-trapped component. Our goal is to provide insights into the long-term evolution of a protoneutron star (PNS) formed after a core-collapse supernova (CCSN) or a remnant resulting from a binary neutron star merger (BNSM). The EOS is derived using a relativistic mean-field quantum many-body theory within the Hartree approximation. C…
Prior work it builds on
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I and JW. Marsden · 2012 · cited 170,903 times · Not summarized yet
Papers that cite it
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Abstract
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Abstract
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Abstract
Every numerical general relativistic investigation starts from the solution of the initial value equations at a given time. Astrophysically relevant initial values for different systems lead to distinct sets of equations that obey specific assumptions tied to the particular problem. Therefore, a robust and efficient solver for a variety of strongly gravitating sources is needed. In this work, we present the OpenMP version of the Compact Object CALculator (COCAL) on shared memory processors. We performed extensive profiling of the core COCAL modules in order to identify bottlenecks in efficiency, which we addressed. Using modest resources, the new parallel code achieves speedups of approximat…
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