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From masses and radii of neutron stars to EOS of nuclear matter through neural network

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Chinese Physics C 2024年第2期48卷 104-111页

作者：武则晗文德华 School of Physics and Optoelectronics South China University of TechnologyGuangzhou 510641China

The equation of state(EOS)of dense nuclear matter is a key factor for determining the internal structure and properties of neutron ***,the EOS of high-density nuclear matter has great uncertainty,mainly because terrestrial nuclear experiments cannot reproduce matter as dense as that in the inner core of a neutron ***,continuous improvements in astronomical observations of neutron stars provide the opportunity to inversely constrain the EOS of high-density nuclear *** methods have been proposed to implement this inverse constraint,including the Bayesian analysis algorithm,the Lindblom’s approach,and so *** network algorithm is an effective method developed in recent *** employing a set of isospin-dependent parametric EOSs as the training sample of a neural network algorithm,we set up an effective way to reconstruct the EOS with relative accuracy using a few mass-radius *** on the obtained neural network algorithms and according to the NICER observations on masses and radii of neutron stars with assumed precision,we obtain the inversely constrained EOS and further calculate the corresponding macroscopic properties of the neutron *** results are basically consistent with the constraint on EOS in Huth et al.[Nature 606,276(2022)]based on Bayesian ***,the results show that even though the neural network algorithm was obtained using the finite parameterized EOS as the training set,it is valid for any rational parameter combination of the parameterized EOS model.

关键词： neutron star neural network equation of state nclear matter D0I:10.1088/1674-1137/ad0e04

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含暗物质中子星性质参量的普适关系研究

原子核物理评论 2024年第1期41卷 331-339页

作者：杨致浩文德华华南理工大学物理与光电学院广州510641

含暗物质中子星是指物质组成中包含了暗物质的中子星。在本文中,我们主要研究了含暗物质中子星性质参量的普适性关系。研究结果表明:与普通中子星结果类似,含暗物质中子星的相关性质参量之间也存在着普适性关系;暗物质粒子质量和含暗物... 详细信息

含暗物质中子星是指物质组成中包含了暗物质的中子星。在本文中,我们主要研究了含暗物质中子星性质参量的普适性关系。研究结果表明:与普通中子星结果类似,含暗物质中子星的相关性质参量之间也存在着普适性关系;暗物质粒子质量和含暗物质质量比例的改变会使含暗物质中子星与普通中子星产生观测上的可区分效应;潮汐形变参数Λ与无量纲引力结合能E_(g)/M、无量纲转动惯量I/M^(3)之间存在指数形式的普适性关系。

关键词：中子星暗物质普适关系

Gravitational waves from the axial oscillation of neutron star considering non-Newtonian gravity

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Nuclear Science and Techniques 2013年第5期24卷 38-43页

作者： wen dehua ZHOU Ying Department of Physics South China University of Technology

The eigen-frequencies of the axial w-modes of neutron star described by a super-soft equation of state(EOS) are investigated,by considering the non-Newtonian *** results show that at the same stellar mass,the frequencies of wI and wI2 for our model are lower than that of the typical EOSs(such as APR); and the frequencies increase with the stellar masses,which is contrary to that of the typical *** characters may provide a probe to testify the super soft symmetry energy and the non-Newtonian gravity in the ***,our model also has the universal behavior of the mass-scaled eigen-frequencies as a function of the compactness.

关键词：非牛顿引力中子星轴向引力波摆动本征频率恒星质量 EOS

Electrically charged: An effective mechanism for soft EOS supporting massive neutron star

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Science China(Physics,Mechanics & Astronomy) 2015年第10期58卷 100-106页

作者： JING ZhenZhen wen dehua ZHANG XiangDong School of Sciences South China University of Technology

The massive neutron star discoverer announced that strange particles, such as hyperons should be ruled out in the neutron star core as the soft Equation of State(EOS) can-not support a massive neutron star. However, many of the nuclear theories and laboratory experiments support that at high density the strange particles will appear and the corresponding EOS of super-dense matters will become soft. This situation promotes a challenge between the astro-observation and nuclear physics. In this work, we introduce an effective mechanism to answer this challenge, that is, if a neutron star is electrically charged, a soft EOS will be equivalently stiffened and thus can support a massive neutron star. By employing a representative soft EOS, it is found that in order to obtain an evident effect on the EOS and thus increasing the maximum stellar mass by the electrostatic field, the total net charge should be in an order of 1020 C. Moreover, by comparing the results of two kind of charge distributions, it is found that even for different distributions, a similar total charge:～2.3×1020C is needed to support a～2.0M⊙neutron star.

关键词： neutron star equation of state electrical field

Constraint on nuclear symmetry energy imposed by f-mode oscillation of neutron stars

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Communications in Theoretical Physics 2021年第11期73卷 122-130页

作者： Jing Zhang dehua wen Yuxi Li School of Physics and Optoelectronics South China University of TechnologyGuangzhou 510641China

Due to improvements in the sensitivity of gravitational wave(GW)detectors,the detection of GWs originating from the fundamental quasi-normal mode(f-mode)of neutron stars has become *** future detection of GWs originating from the f-mode of neutron stars will provide a potential way to improve our understanding of the nature of nuclear matter inside neutron *** this work,we investigate the constraint imposed by the f-mode oscillation of neutron stars on the symmetry energy of nuclear matter using Bayesian analysis and parametric *** is shown that if the frequency of the f-mode of a neutron star of known mass is observed precisely,the symmetry energy at twice the saturation density(E_(sym)(2_(ρ0)))of nuclear matter can be constrained within a relatively narrow *** example,when all the following parameters are within the given intervals:220≤K0≤260 Me V,28≤E_(sym)(ρ0)≤36 Me V,30≤L≤90 Me V,-800≤J0≤400 Me V,-400≤K_(sym)≤100 Me V,-200≤Jsym≤800 Me V,E_(sym)(2ρ0)will be constrained to within-+48.***.56.6 Me V if the f-mode frequency of a canonical neutron star(1.4 M■)is observed to be 1.720 k Hz with a 1%relative ***,if only f-mode frequency detection is available,*** is no stellar mass measurement,a precisely detected f-mode frequency can also impose an accurate constraint on the symmetry *** example,given the same parameter space and the same assumed observed f-mode frequency mentioned above,and assuming that the stellar mass is in the range of 1.2–2.0 Me,E_(sym)(2ρ0)will be constrained to within 49.5■*** addition,it is shown that a higher slope of 69≤L≤143 Me V will give a higher posterior distribution of E_(sym)(2ρ0),53.8■MeV.

关键词： f-mode Bayesian analysis nuclear symmetry energy neutron star

Suitable resolution of EOS tables for neutron star investigations

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Chinese Physics C 2019年第5期43卷 93-98页

作者： Houyuan Chen dehua wen Na Zhang School of Physics and Optoelectronics South China University of Technology

Inasmuch as the hydrostatic structure of the interior of neutron stars uniquely depends on the equation of state(EOS), the inverse constraints on EOS from astrophysical observations have been an important method for revealing the properties of high density matter. Currently, most EOS for neutron star matter are given in tabular form,but these numerical tables can have quite different resolution. To guarantee both the accuracy and efficiency in computing the Tolman-Oppenheimer-Volkoff equations, a concise standard for generating EOS tables with suitable resolution is investigated. It is shown that EOS tables with 50 points logarithmic-uniformly distributed in the supra-nuclear density segment [ρ_0, 10_(ρ0)], where ρ_0 is the nuclear saturation density, correspond to the interpolation induced errors of ～0.02% for the gravitational mass M and ～0.2% for the tidal deformability ∧.

关键词： neutron star equation of state TOV equations

Effect of Fe_(2)O_(3)on the Structure,Physical Properties and Crystallization of CaO-Al_(2)O_(3)-SiO_(2)Glass

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Journal of Wuhan University of Technology(Materials Science) 2024年第4期39卷 954-961页

作者：张峰 XIONG dehua 谢俊张继红 HAN Jianjun CHEN Dequan wen Zhongquan FAN Zhenhua CHEN Lina SUN Tengfei State Key Laboratory of Silicate Materials for Architectures Wuhan University of TechnologyWuhan 430070China Hepu Research Center for Silicate Materials Industry Technology Beihai 536100China Hainan Institute of Wuhan University of Technology Sanya 430079China Shenzhen Research Institute of Wuhan University of Technology Shenzhen 518000China Chongqing Polycomp Inter-national Corporation Chongqing 400400China

The calcium aluminosilicate-based glasses(CaO-Al_(2)O_(3)-SiO_(2),CAS)with different Fe_(2)O_(3)content(0.10wt%,0.50wt%,0.90wt%,and 1.30wt%)were prepared by traditional melt-quenching *** glass network structure,thermal and mechanical properties,and crystallization behavior changes were investigated by nuclear magnetic resonance spectrometer,Fourier-transform infrared spectro-photometer,X-ray diffractometer,differential scanning calorimetry and field emission scanning electron microscope *** change of Q^(n)in glass structures reveals the glass network connectivity decreases due to the increasing content of Fe_(2)O_(3)addition,resulting in the increasing of non-bridging number in glass *** glass densities slightly rise from 2.644 to 2.681 g/cm^(3),while Vickers’s hardness increases at first,from 6.469 to 6.901 GPa,then slightly drops to 6.745 GPa,with Fe_(2)O_(3)content *** is almost no thermal expansion coefficient change from different Fe_(2)O_(3)*** glass transmittance in visible range gradually decreases with higher Fe_(2)O_(3)content,resulting from the strong absorption of Fe^(2+)and Fe^(3+)*** calculated activation energy from thermal analysis results first decreases from 282.70 to 231.18 kJ/mol,and then increases to 244.02 kJ/mol,with the Fe_(2)O_(3)content increasing from 0.10wt%to 1.30wt%.Meanwhile,the maximum Avrami constant of 2.33 means the CAS glasses exhibit two-dimensional *** of the CAS glass-ceramics samples contain main crystal phase of anorthite,the microstructure appears lamellar and columnar crystals.

关键词： calcium aluminosilicate glass network structure physical properties crystallization

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施工与运营初期厚表土立井井壁受力实测研究

中国工程科学 2012年第2期14卷 80-84页

作者：温德华上海大屯能源股份有限公司江苏沛县221000

采用井筒内外井壁现场埋设传感器的方法,建立由计算机控制的自动监测系统,实测大屯矿区某混合井井壁施工过程及之后一段时间的受力和变形演变规律。对实测结果进行分析,研究内外井壁的综合变形规律,可以预测井壁的长期安全性,为井壁破... 详细信息

采用井筒内外井壁现场埋设传感器的方法,建立由计算机控制的自动监测系统,实测大屯矿区某混合井井壁施工过程及之后一段时间的受力和变形演变规律。对实测结果进行分析,研究内外井壁的综合变形规律,可以预测井壁的长期安全性,为井壁破裂的预防和治理提供科学决策的依据。

关键词：井壁监测厚表土应变附加力

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局域物态方程对中子星整体性质的影响

原子核物理评论 2018年第3期35卷 264-269页

作者：张娜文德华华南理工大学物理与光电学院广州510641

由于高密非对称核物质核核相互作用的复杂性,使得目前人们对高密非对称核物质的物态方程的认识还存在很大的不确定性。利用逐段修改物态方程的方法,探究了不同密度段物态方程对中子星整体性质的影响,尤其是对典型中子星(1.4 M_⊙)半径... 详细信息

由于高密非对称核物质核核相互作用的复杂性,使得目前人们对高密非对称核物质的物态方程的认识还存在很大的不确定性。利用逐段修改物态方程的方法,探究了不同密度段物态方程对中子星整体性质的影响,尤其是对典型中子星(1.4 M_⊙)半径及最大质量的影响。研究进一步证实了在2倍饱和核密度附近的物态方程对典型质量中子星的半径有显著影响。还进一步分析了中子星的质量半径关系曲线特征及其斜率(dM/dR)对物态方程的依赖性,发现d M/d R主要由饱和核密度以上的中子星物质的物态方程决定。探索不同密度段物态方程对中子星整体性质的影响以及探索dM/dR对物态方程的依赖性,主要是为将来利用中子星的天文观测来反向约束致密物质的物态方程提供理论参考。

关键词：中子星物态方程质量-半径关系