arXiv subjects

Xuhao Wu

Publications and source records attributed to Xuhao Wu.

13 recordsLinked to original sources

arXiv2026

The mixed phase quark core in massive hybrid stars

We investigate the properties of hybrid star and the mixed phase core to explore the radius ratio of the mixed phase in hybrid star. In the context of observed massive neutron stars (NSs), we examine the internal structure, phase transitions, and the impacts of the equation of state (EOS) in maximum hybrid star. We investigate the stiffness changes in the EOS during the hadron-quark phase transition within the hybrid stars. The relativistic mean-field (RMF) model is used to describe hadronic matter, while to the represent quark matter, the Nambu-Jona-Lasinio (NJL) model is applied. We explore the strength of vector coupling in quark matter, which delays the onset density of the mixed phase and reduces the size of the mixed-phase core in a hybrid star, but does not exhibit a clear correlation with the central density. In a hybrid star with a maximum mass of approximately 2 solar masses ($M_\odot$), a mixed-phase core of $\sim$5 km may exist, comprising about $40\%$ of the total radius. However, our results do not support the existence of a sizable quark core containing the mixed phase ($R_{\rm{MP}}>1/2~R_{\rm{total}}$) for the maximum-mass hybrid star or for a 2~$M_\odot$ massive star.

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arXiv2026

Properties of H particle-admixed compact star

We explore the potential manifestation of a hexaquark, the H particle, as a constituent within neutron stars. The H particle, characterized by a quark composition of $uuddss$, is constructed using the framework of Chromomagnetic Interaction (CMI). Specifically, we contemplate the flavor-singlet state H with $J^P=0^+$. Our computations indicate that the three-flavor hexaquark state, the H particle, possesses a lower mass of $2212.7~\rm{MeV}$ in comparison to the $d^*(2380)$, implying greater stability than the two-flavor $d^*(2380)$. The analysis involving the H particle is carried out using the relativistic mean-field (RMF) model. We investigate the influence of H particle couplings, a key factor in determining the system stability, and focus on the potential existence of H particle within neutron stars. We find that H particle could potentially endure as a stable constituent within neutron stars, and lead to a reduction of the maximum mass.

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arXiv2025

ENLighten: Lighten the Transformer, Enable Efficient Optical Acceleration

Photonic computing has emerged as a promising substrate for accelerating the dense linear-algebra operations at the heart of AI, yet adoption for large Transformer models remains in its infancy. We identify two bottlenecks: (1) costly electro--optic conversions and data-movement overheads that erode energy efficiency as model sizes scale; (2) a mismatch between limited on-chip photonic resources and Transformer scale, which forces frequent reuse of photonic tensor cores and dilutes throughput gains. To address these challenges, we introduce a hardware--software co-design framework. First, we propose \texttt{Lighten}, a PTC-aware compression flow that post-hoc decomposes each Transformer weight matrix into a low-rank component plus a structured-sparse component aligned to photonic tensor-core granularity, without lengthy retraining. Second, we present \texttt{ENLighten}, a reconfigurable photonic accelerator with dynamically adaptive tensor cores, driven by broadband light redistribution, enabling fine-grained sparsity support and full power gating of inactive parts. On ImageNet, \texttt{Lighten} prunes a Base-scale Vision Transformer by 50\% with $\approx$1\% accuracy drop after only 3 epochs (about 1 hour) of fine-tuning. Deployed on \texttt{ENLighten}, it achieves a $2.5\times$ improvement in energy--delay product over the state-of-the-art photonic Transformer accelerator.

cs.ET↗

arXiv2025

Effects of symmetry energy on the properties of hadron-quark mixed phase in hybrid stars

We study how the nuclear symmetry energy slope affects the properties of hadron-quark pasta phases and their sizes in massive hybrid stars ($> 2 M_{\odot}$). We utilize the relativistic mean-field model with a density-dependent isovector coupling constant fitted by varying values of the symmetry energy slope $L$ to describe the hadronic matter, while the quark matter is described by a modified MIT bag model with vector interactions. We construct the hadron-quark phase transition using the energy minimization (EM) method and compare with the Gibbs construction (GC) in the hybrid star. We find that the massive hybrid stars generally tend to have a hadron-quark pasta phase core rather than a pure quark core for most values of $L$, except in some special cases where they have a small pure quark core. Furthermore, we show that the mass and size of the pasta phase core are strongly influenced by the symmetry energy. The radius associated with the onset of pasta phases is also influenced by the symmetry energy. Additionally, we also evaluate the effects of the surface tension $σ$, the bag constant $B$, and the vector interaction $G_{V}$.

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arXiv2025

HESS J1731-347 is likely a Quark Star Based on the Density-Dependent vMIT Bag Model

In this study, we extend the MIT bag model by incorporating the vector interaction among quarks and introducing a density-dependent bag pressure.Then we proceed to investigate the thermodynamic properties of strange quark matter (SQM) and pure up-down quark matter (udQM) in quark stars (QSs).Our findings demonstrate that the density dependence of bag pressure $B(n_b)$ and the vector interaction $G_V$ among quarks can significantly stiffen the equation of state (EOS) for both SQM and udQM which allows for the description of massive compact stars such as those observed in GW190814 and PSR J0740+6620 as plausible candidates for QSs.Ultimately, we derived a series of mass-radius relations of QS based on several combinations of ($B_{as}$, $β$). Our results support the hypothesis that HESS J1731-347 is a quark star.

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arXiv2023

Cosmic QCD transition-from quark to strangeon and nucleon

A crossover QCD phase transition in the early Universe, involving a formation scenario of stable strangeon nuggets is studied. The Polyakov-Nambu-Jona-Lasinio model is applied to calculate the thermodynamics of the QCD phase with u, d, s quarks, and the relativistic mean-field model describes the hadronic matter. The crossover phase transition from quarks to hadrons occurred at cosmic temperature of T~170 MeV, and those two phases are connected in a three-window model. Due to quark's non-perturbative coupling, quark clusters with net strangeness (i.e., strangeons) and then strangeon nuggets could form during the transition process. A distribution function of the nugget baryon number, A, is introduced to describe the nuggets' number density. All the strangeon nuggets with A>A_c are considered to be stable, where the critical number, A_c, is determined by both the weak and strong interactions. A non-relativistic equation of state is applied to calculate the thermodynamics of stable nuggets. The calculation shows that the thermodynamical contributions (pressure, entropy, etc.) of the stable strangeon nuggets are negligible. The resultant mass density of the strangeon nuggets survival from the early Universe is comparable to the dark matter, that indicates a possible explanation of the cold dark matter without introducing any exotic particles beyond the standard model.

hep-ph↗

arXiv2021

Hadron-quark mixed phase in the quark-meson coupling model

We explore the possibility of a structured hadron-quark mixed phase forming in the interior of neutron stars. The quark-meson coupling (QMC) model, which explicitly incorporates the internal quark structure of the nucleon, is employed to describe the hadronic phase, while the quark phase is described by the same bag model as the one used in the QMC framework, so as to keep consistency between the two coexisting phases. We analyze the effect of the appearance of hadron-quark pasta phases on the neutron-star properties. We also discuss the influence of nuclear symmetry energy and the bag constant B in quark matter on the deconfinement phase transition. For the treatment of the hadron-quark mixed phase, we use the energy minimization method and compare it with the Gibbs construction. The finite-size effects like surface and Coulomb energies are taken into account in the energy minimization method; they play crucial roles in determining the pasta configuration during the hadron-quark phase transition. It is found that the finite-size effects can significantly reduce the region of the mixed phase relative to that of the Gibbs construction. Using a consistent value of B in the QMC model and quark matter, we find that hadron-quark pasta phases are formed in the interior of massive stars, but no pure quark matter can exist.

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arXiv2021

Symmetry energy effect on the secondary component of GW190814 as a neutron star

The secondary component of GW190814 with a mass of 2.50-2.67 $M_{\odot}$ may be the lightest black hole or the heaviest neutron star ever observed in a binary compact object system. To explore the possible equation of state (EOS), which can support such massive neutron star, we apply the relativistic mean-field model with a density-dependent isovector coupling constant to describe the neutron-star matter. The acceptable EOS should satisfy some constraints: the EOS model can provide a satisfactory description of the nuclei; the maximum mass $M_\textrm{TOV}$ is above 2.6 $M_{\odot}$; the tidal deformability of a canonical 1.4 $M_{\odot}$ neutron star $Λ_{1.4}$ should lie in the constrained range from GW170817. In this paper, we find that the nuclear symmetry energy and its density dependence play a crucial role in determining the EOS of neutron-star matter. The constraints from the mass of 2.6 $M_{\odot}$ and the tidal deformability $Λ_{1.4}=616_{-158}^{+273}$ (based on the assumption that GW190814 is a neutron star-black hole binary) can be satisfied as the slope of symmetry energy $L \leq 50$ MeV. Even including the constraint of $Λ_{1.4}=190_{-120}^{+390}$ from GW170817 which suppresses the EOS stiffness at low density, the possibility that the secondary component of GW190814 is a massive neutron star cannot be excluded in this study.

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arXiv2020

The geometry and environment of repeating FRBs

We propose a geometrical explanation for periodically and nonperiodically repeating fast radio bursts (FRBs) under neutron star (NS)-companion systems. We suggest a constant critical binary separation, $r_{\rm c}$, within which the interaction between the NS and companion can trigger FRB bursts. For an elliptic orbit with the minimum and maximum binary separations, $r_{\rm min}$ and $r_{\rm max}$, a periodically repeating FRB with an active period could be reproduced if $r_{\rm min}<r_{\rm c}<r_{\rm max}$. However, if $r_{\rm max}<r_{\rm c}$, the modulation of orbital motion will not work due to persistent interaction, and this kind of repeating FRBs should be nonperiodic. We test relevant NS-companion binary scenarios on the basis of FRB 180916.J0158+65 and FRB 121102 under this geometrical frame. It is found that the pulsar-asteroid belt impact model is more suitable to explain these two FRBs since this model is compatible with different companions (e.g., massive stars and black holes). At last, we point out that FRB 121102-like samples are potential objects which can reveal the evolution of star-forming region.

astro-ph.HE↗

arXiv2020

What if the neutron star maximum mass is beyond $\sim2.3 M_{\odot}$?

By assuming the formation of a black hole soon after the merger event of GW170817, Shibata et al. updated the constraints on the maximum mass ($M_\textrm{max}$) of a stable neutron star within $\lesssim$ 2.3 $M_{\odot}$, but there is no solid evidence to rule out $M_\textrm{max}>2.3~M_{\odot}$ from the point of both microphysical and astrophysical views. In order to explain massive pulsars, it is naturally expected that the equation of state (EOS) would become stiffer beyond a specific density. In this paper, we consider the possibility of EOSs with $M_\textrm{max}>2.3~M_{\odot}$, investigating the stiffness and the transition density in a polytropic model. Two kinds of neutron stars are considered, i.e., normal neutron stars (the density vanishes on gravity-bound surface) and strange stars (a sharp density discontinuity on self-bound surface). The polytropic model has only two parameter inputs in both cases: ($ρ_{\rm t}$, $γ$) for gravity-bound objects, while ($ρ_{\rm s}$, $γ$) for self-bound ones, with $ρ_{\rm t}$ the transition density, $ρ_{\rm s}$ the surface density and $γ$ the polytropic exponent. In the matter of $M_\textrm{max}>2.3~M_{\odot}$, it is found that the smallest $ρ_{\rm t}$ and $γ$ should be $\sim 0.50~ρ_0$ and $\sim 2.65$ for normal neutron stars, respectively, whereas for strange star, we have $γ> 1.40$ if $ρ_{\rm s} > 1.0~ρ_0$ and $ρ_{\rm s} < 1.58~ρ_0$ if $γ<2.0$ ($ρ_0$ is the nuclear saturation density). These parametric results could guide further research of the real EOS with any foundation of microphysics if a pulsar mass higher than $2.3~M_{\odot}$ is measured in the future. We also derive rough results of common neutron star radius range, which is $9.8~\rm{km} < R_{1.4} < 13.8~\rm{km}$ for normal neutron stars and $10.5~\rm{km} < R_{1.4} < 12.5~\rm{km}$ for strange stars.

astro-ph.HE↗

arXiv2019

Quark matter symmetry energy effect on equation of state for neutron stars

We study the equation of state of neutron-star matter including the effects of isovector-vector coupling in quark matter. We employ the relativistic mean-field theory with an extended TM1 parameter set to describe hadronic matter and the SU(3) Nambu-Jona-Lasinio model with isovector-vector and hypercharge-vector couplings to describe the quark matter. The deconfinement hadron-quark phase transition is constructed under Gibbs phase equilibrium conditions. It is found that the isovector-vector and hypercharge-vector couplings in quark matter enhance the symmetry energy and hypercharge symmetry energy in neutron-star matter.

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arXiv2018

Effects of quark-matter symmetry energy on hadron-quark coexistence in neutron-star matter

We examine the effects of the isovector-vector coupling and hypercharge-vector coupling in quark matter on hadron-quark coexistence in neutron-star matter. The relativistic mean field theory with the TM1 parameter set and an extended TM1 parameter set are used to describe hadronic matter, and the Nambu-Jona-Lasinio model with scalar, isoscalar-vector, isovector-vector and hypercharge-vector couplings is used to describe deconfined quark matter. The hadron-quark phase transition is constructed via the Gibbs conditions for phase equilibrium. The isovector-vector and hypercharge-vector couplings in quark matter enhance the symmetry energy and hypercharge symmetry energy in neutron-star matter, while their effects are found to be suppressed at high densities by the strange quarks. As a result, the hadron-quark mixed phase shrinks with only isovector-vector coupling and moves to higher density with isovector-vector and hypercharge-vector couplings. The maximum mass of neutron-star increases slightly with isovector-vector and hypercharge-vector couplings.

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arXiv2017

Finite-size effects on the hadron-quark phase transition in neutron stars

We study the finite-size effects, like the surface and Coulomb energies, on the hadron-quark mixed phase in neutron stars. The equilibrium conditions for coexisting hadronic and quark phases are derived by minimizing the total energy including the surface and Coulomb contributions, which are different from the Gibbs conditions without finite-size effects. We employ the relativistic mean-field model to describe the hadronic phase, while the Nambu-Jona-Lasinio model with vector interactions is used for the quark phase. It is found that finite-size effects can significantly reduce the region of the mixed phase, and the results lie between those of the Gibbs and Maxwell constructions. We show that a massive star may contain a mixed-phase core and its size depends on the surface tension of the hadron-quark interface and the vector coupling between quarks. The repulsive vector interaction in the Nambu-Jona-Lasinio model can stiffen the equation of state of quark matter, and therefore, delay the phase transition and increase the maximum mass of neutron stars.

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