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Dark energy effects on surface gravitational redshift and Keplerian frequency of neutron stars

Communications in Theoretical Physics 2025年第1期77卷 122-129页

作者： Jia-Jing He Yan Xu Yi-Bo Wang Xiu-Lin Huang Xing-Xing Hu Yu-Fu Shen Changchun Observatory National Astronomical ObservatoriesChinese Academy of SciencesChangchun 130117China School of Astronomy and Space Sciences University of Chinese Academy of SciencesBeijing 100049China

Research on the properties of neutron stars with dark energy is a particularly interesting yet unresolved problem in *** analyze the influence of dark energy on the equation of state,the maximum mass,the surface gravitational redshift and the Keplerian frequency for the traditional neutron star and the hyperon star matter within the relativistic mean field theory,using the GM1 and TM1 parameter sets by considering the two flavor symmetries of SU(6)and SU(3)combined with the observations of PSR J1614-2230,PSR J0348+0432,PSR J0030+0451,RX J0720.4-3125,and 1E *** is found that the existence of dark energy leads to the softened equations of the state of the traditional neutron star and the hyperon *** radius of a fixed-mass traditional neutron star(or hyperon star)with dark energy becomes smaller,which leads to increased *** existence of dark energy can also enhance the surface gravitational redshift and the Keplerian frequency of traditional neutron stars and hyperon *** growth of the Keplerian frequency may cause the spin rate to speed up,which may provide a possible way to understand and explain the pulsar glitch ***,we infer that the mass and the surface gravitational redshift of PSR J1748-2446ad without dark energy for the GM1(TM1)parameter set are 1.141 M_(☉)(1.309 M_(☉))and 0.095(0.105),*** corresponding values for the GM1(TM1)parameter set are 0.901 M_(☉)(1.072M_(☉))and 0.079(0.091)if PSR J1748-2446ad contains dark energy withα=*** J1748-2446ad may be a low-mass pulsar with a lower surface gravitational redshift under our selected models.

关键词： dark energy neutron stars gravitational redshift Keplerian frequency

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Axion Gamma-Ray Signatures from Quark Matter in neutron stars and Gravitational Wave Comparisons

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Journal of Modern Physics 2025年第1期16卷 152-166页

作者： Bijan Berenji SLAC National Accelerator Laboratory Menlo Park CA USA

We present a theoretical model for detecting axions from neutron stars in a QCD phase of quark matter. The axions would be produced from a quark-antiquark pair uu¯or dd¯, in loop(s) involving gluons. The chiral anomaly of QCD and the spontaneously broken symmetry are invoked to explain the non-conservation of the axion current. From the coupling form factors, the axion emissivities ϵacan be derived, from which fluxes can be determined. We predict a photon flux, which may be detectable by Fermi LAT, and limits on the QCD mass ma. In this model, axions decay to gamma rays in a 2-photon vertex. We may determine the expected fluxes from the theoretical emissivity. The sensitivity curve from the Fermi Large Area Telescope (Fermi LAT) would allow axion mass constraints for neutron stars as low as ma≤10−14eV 95% C.L. Axions could thus be detectable in gamma rays for neutron stars as distant as 100 kpc. A signal from LIGO GWS 170817 could be placed from the NS-NS merger, which gives an upper limit of ma≤10−10eV.

关键词： Astrophysics Phenomenology QCD Axion neutron stars Nuclear Theory Gamma Rays Gravitational Waves Fermi-LAT

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neutron stars including the effects of chaotic magnetic fields and anomalous magnetic moments

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Chinese Physics C 2017年第4期41卷 117-123页

作者：吴飞吴琛任中洲 Physics Department Nanjing University Shanghai Institute of Applied Physics Chinese Academy of Science Center of Theoretical Nuclear Physics National Laboratory of Heavy-Ion Accelerator Kavli Institute for Theoretical Physics China Chinese Academy of Sciences

The relativistic mean field（RMF） FSUGold model extended to include hyperons is employed to study the properties of neutron stars with strong magnetic *** chaotic magnetic field approximation is *** effect of anomalous magnetic moments（AMMs） is also *** is shown that the equation of state（EOS）of neutron star matter is stiffened by the presence of the magnetic field,which increases the maximum mass of a neutron star by around 6%.The AMMs only have a small influence on the EOS of neutron star matter,and increase the maximum mass of a neutron star by 0.02M（sun）.Neutral particles are spin polarized due to the presence of the AMMs.

关键词： magnetic field neutron stars equation of state

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The role of magnetic damping in the r-mode evolution of accreting neutron stars

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Science China(Physics,Mechanics & Astronomy) 2015年第3期58卷 90-95页

作者： CAO GuoJie ZHOU Xia WANG Na Xinjiang Astronomical Observatory Chinese Academy of Sciences University of Chinese Academy of Sciences Key Laboratory of Radio Astronomy Chinese Academy of Sciences

The magnetic damping rate was introduced in the evolution equations of r-modes,which shows that r-modes can generate strong toroidal magnetic fields in the core of accreting millisecond pulsars inducing by differential *** consideration of the coupling evolution of r-modes,spin and thermal evolution,we investigated the influence of the magnetic damping on the differential rotation of nonlinear r-modes of accreting neutron *** derived the coupling evolution equations of the star involving the magnetic damping rate in the framework of second-order r-mode *** numerical results show that the magnetic damping suppressed the nonlinear evolution of r-modes since the saturation amplitude is reduced to a great *** particular,because of the presence of the generated toroidal magnetic field,the spin-down of the stars is terminated and the viscous heating effects are also ***,we could obtain a stronger generated toroidal magnetic field in the second-order r-mode *** gravitational radiation may be detected by the advanced laser interferometer detector LIGO if the amount of differential rotation is small when the r-mode instability becomes active and the accretion rate is not very high.

关键词： neutron stars r-mode instability differential rotation gravitational waves

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Influence of the nuclear equation of state on the hadron-quark phase transition in neutron stars

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Chinese Physics C 2008年第7期32卷 536-542页

作者：杨芳申虹 Department of Physics Nankai UniversityTianjin 300071China

We study the hadron-quark phase transition in the interior of neutron stars, and examine the influence of the nuclear equation of state on the phase transition and neutron star properties. The relativistic mean field theory with several parameter sets is used to construct the nuclear equation of state, while the Nambu-Jona-Lasinio model is used for the description of the deconfined quark phase. Our results show that a harder nuclear equation of state leads to an earlier onset of a mixed phase of hadronic and quark matter. We find that a massive neutron star possesses a mixed phase core, but it is not dense enough to possess a pure quark core.

关键词： hadron-quark phase transition equation of state neutron stars

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Effects of relativistic parameter sets on tidal deformabilities and f-mode oscillations of neutron stars

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Communications in Theoretical Physics 2022年第6期74卷 87-102页

作者： Bin Hong Xue-Ling Mu School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Key Laboratory of Modern Astronomy and Astrophysics(Nanjing University) Ministry of EducationNanjing 210023China College of Electronic Information and Electrical Engineering Chengdu UniversityChendu 610106China

The implications of relativistic parameter sets established at saturation density on the tidal deformabilities and f-mode oscillations of neutron stars(NSs)are examined using constraints from the gravitational wave(GW)event GW170817 and *** to our findings,the isovector saturation parameters have a greater impact on the radii and tidal deformabilities of NSs than the isoscalar saturation *** analysis also examines the impact of saturation properties on f-mode frequencies and finds that f-mode frequencies with 1.4 M⊙(solar mass)are roughly between 1.95 and 2.15 *** findings could be confirmed by future advanced GW detectors.A good linear parameter-independent correlation between f-mode frequencies inferred from saturation parameters in the entire region is also observed,and we attempt to fit an updated version of this universal ***,we used chiral effective theory(χEFT)together with the multi-messenger astronomy constraints to further reinforce the rationality of the conclusions we have reached.

关键词： neutron stars nuclear astrophysics massive stars

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Systematic comparison of initial velocities for neutron stars in different models

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Research in Astronomy and Astrophysics 2016年第7期16卷 1-8页

作者： Ali Taani Applied Science Department Aqaba University College Aqaba Al-Balqa' Applied University RO. Box 1199 77110Salt Jordan Department of Applied Physics and Astronomy University of Sharjah P.O. Box 27272 Sharjah United Arab Emirates

I have studied the initial velocity（Maxwellian and exponential distributions） and the scale height of isolated old（aged≥10^9yr） neutron stars（NSs） at different Galactocentric distances R in three population models. The smooth time-independent 3-D axisymmetric gravitational potentials（MiyamotoNagai and Paczy n′ski models） were also used. The correlation between these quantities significantly affects the shapes of the profiles and distributions of the simulated sample, because the differences in the initial kick can arise from differences in the formation and evolution of NSs with other physical parameters. The scale height of the density distribution increases systematically with R. I have also shown that the distribution of old NSs in these population models agrees with the observed structure of the Galaxy in terms of initial velocities（1-D and 3-D）, as well as the scale height distributions. These distributions tend to have an asymptotic behavior at the point R = 2.75 kpc. This means that the quality of the models can be described in terms of a mean of the fitted Gaussian, and this could also give an overall perspective of the phase space properties of nearby old NSs on a given gravitational potential.

关键词： pulsar general stars neutron stars statistics stars evolution Galaxy structure Galaxy disk galaxies kinematics and dynamics

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Knotted Solitons in an Interacting Mixture of a Charged and a Neutral Superfluid for neutron stars

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Communications in Theoretical Physics 2009年第9期52卷 555-560页

作者： REN Ji-Rong GUO Heng ZHANG Xin-Hui LI Ran Institute of Theoretical Physics Lanzhou University Lanzhou 730000 China

By making use of the decomposition of U（1） gauge potential theory and the C-mapping method we discuss a mixture of interacting neutral and charged Bose condensates, which is supposed being realized in the interior of neutron stars in the form of a coexistent neutron superfluid and protonic superconductor. We propose that this system possesses vortex lines and two classes of knotted solitons. The topological charge of the vortex lines are characterized by the Hopf indices and the Brower degrees of φ-mapping, and the knotted solitons are described by nontrivial Hopf invariant and the BF action respectively.

关键词： neutron stars topological excitations spontaneous breaking of gauge symmetries

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Key factor for determining relation between radius and tidal deformability of neutron stars: Slope of symmetry energy

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Chinese Physics C 2020年第6期44卷 103-108页

作者： Nai-Bo Zhang Bin Qi Shou-Yu Wang Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment School of Space Science and PhysicsInstitute of Space SciencesShandong UniversityWeihai 264209China

The constraints on tidal deformability Λ of neutron stars were first extracted from GW170817 by LIGO and Virgo ***,the relationship between the radius R and tidal deformability Λ is still under *** an isospin-dependent parameterized equation of state(EOS),we study the relation between R andΛand its dependence on parameters of symmetry energy Esym and EOS of symmetric nuclear matter E0 when the mass is fixed at 1.4 M⊙,1.0 M⊙,and 1.8 M⊙.We find that,although the changes of high order parameters of Esym and E 0 can shift individual values of R1.4 and Λ1.4,the R1.4~Λ1.4 relation remains approximately at the same fitted *** slope L of the symmetry energy plays the dominant role in determining the R1.4~Λ1.4 *** investigating the mass dependence of the R~Λ relation,we find that the well fitted R~Λ relation for 1.4 M⊙ is broken for massive neutron stars.

关键词： neutron stars symmetry energy tidal deformability radius

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The spatial distribution of old neutron stars in the Galaxy

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Science China(Physics,Mechanics & Astronomy) 2010年第10期53卷 1939-1946页

作者： WEI YingChun ZHANG ChengMin WU XinJi ZHAO YongHeng CHOU ChiKang LUO ALi National Astronomical Observatories Chinese Academy of SciencesBeijing 100012China Department of Astronomy Peking UniversityBeijing 100871China National Astronomical Observatories/Urumqi Observatory Chinese Academy of SciencesUrumqi 830011China

The spatial distributions of old neutron stars (NSs) with ages 109 to 1010 yr in our Galaxy are investigated by Monte Carlo simulation under two different initial random velocity *** is found that the scale heights of the distribution increase with the Galactic radial *** location of the peak of the NS distribution is closer to the Galactic center than that of their *** results from our detailed numerical analysis reveal that there is resemblance between the simulated old NS distribution and the structure of the observed HI disk.

关键词： neutron stars Galaxy structure Galaxy disk star evolution

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