利用含δ介子的相对论平均场理论研究中子星潮汐形变性质

开展中子星宏观性质的研究,对于揭示中子星内部组成和结构具有重要意义.本文基于相对论平均场理论模型,研究了δ介子对传统中子星和超子星物态方程、最大质量、勒夫数和潮汐形变能力的影响.结果表明,对于中小质量传统中子星(或超子星), δ介子使其潮汐形变能力变强;随着传统中子星(或超子星)质量的增加, δ介子对其潮汐形变能力影响逐渐减弱;尤其对于大质量超子星,含有δ介子的超子星潮汐形变能力相比不含δ介子的超子星变弱.此外,在相同质量下超子的存在会降低星体的潮汐形变能力,在本文所选的参数下,含有δ介子的星体中,仅同时含L,Σ和Ξ超子的超子星潮汐形变能力能同时满足GW170817和GW190814天文观测约束.随着与中子星相关的引力波数据逐渐增加,将为人们判断超子星内超子种类提供一个可能的途径.     

Nucleonic ~1S_0 Superfluidity Induced by a Soft Pion in Neutron Star Matter with Antikaon Condensations

The nucleonic ~1S_0 superfluidity is investigated by solving the gap equation for the Reid soft-core potential as the nucleon-nucleon interaction in neutron star(NS) matter which is considered to be made up of p, e, μ and condensed antikaon matter. We mainly study the influence of the soft pion-induced potential on the nucleonic~1S_0 pairing gaps in the above NS matter. It is found that the intensities of the nucleonic ~1S_0 pairing gaps including the soft pion-induced potential are smaller than those calculated in the case of not including the soft pion-induced potential. Furthermore, the nucleonic ~1S_0 pairing gaps with the soft pion-induced potential fall into decline with the deepening of the optical potential of antikaons in the above NS matter, whereas they increase with the parameter η for the fixed optical potential of antikaons. Due to the appearance of the soft pion-induced potential, the maximum values of nucleonic ~1S_0 pairing gaps at parameter η = 0.20,0.55 are suppressed by1.7%-6.8% with respect to the case without soft pion-induced potential in the above NS matter.     

Effects of a Weakly Interacting Light U Boson on Protoneutron Stars Including the Hyperon-Hyperon Interactions

In the framework of the relativistic mean field theory including the hyperon-hyperon(YY) interactions,protoneutron stars with a weakly interacting light U boson are studied. The U-boson leads to the increase of the star maximum mass. The modification to the maximum mass by the U-boson with the strong YY interaction is larger than that with the weak YY interaction. The maximum mass of the protoneutron star is less sensitive to the U-boson than that of the neutron star. The inclusion of the U-boson narrows down the mass window for the hyperonized protoneutron stars. As g~2/μ~2 increases, the species of hyperons, which can appear in a stable protoneutron star decrease. The rotation frequency, the red shift, the momentum of inertia and the total neutrino fraction of PSR J1903-0327 are sensitive to the U-boson and change with g~2/μ~2 in an approximate linear trend. The possible way to constrain the coupling constants of the U-boson is discussed.     

基于眼模型的折/衍混合眼底相机设计

应用二元衍射光学理论,设计了一个基于Gullstrand-LeGrand眼光学模型的折／衍混合免散瞳手持式数字眼底相机．该相机的视场角28°,摄影系统由五片透镜构成,其中包含一个二元面．在综合考虑人眼本身和外部系统的像差后,实现了全视场200万像素的高清晰成像,具有较大调焦能力,对-10D至7D屈光度人眼普遍适用．结果显示,该系统成像分辨率高于120lp／mm,场曲值小于0．75mm,畸变仅为7．0％,色差小于3．5μm．衍射光学元件的引入,有效地简化了系统,减小了重量和体积．     

β-环糊精增敏荧光法测定果蔬中呋喃丹的残留量

利用荧光光谱法探讨了β-环糊精与呋喃丹间的超分子相互作用,证明β-环糊精与呋喃丹可形成1:1的超分子包合物,在λex/λem=272/323 nm处发射强荧光,包合常数为108.2 L·mol-1。据此建立了测定水溶液中呋喃丹的荧光分析新方法。在0.0025～0.03μg/mL范围内,呋喃丹的荧光强度与浓度呈良好的线性关系,相关系数R=0.9990,方法的检出限为0.0013μg/mL,相对标准偏差为1.2%。该体系的抗干扰能力及稳定性好,实际样品分析回收率为98%～102%。     

K^- Condensation in Neutron Star Matter with △ Quartet

In the framework of relativistic mean field theory, the condensations of K^- and K^0 in neutron star matter including baryon octet and △ quartet are studied. We find that in this case K^- and K^0 condensations can occur at relative shallow optical potential depth of K^ from -80 MeV to -160 MeV. Both K^- and K^0 condensations favor the appearances of △ resonances. With K^- condensations all the △ quartet can appear well inside the maximum mass stars. The appearances of △ resonances change the composition and distribution of particles at high densities. The populations of △ resonances can enhance K^- condensation. It is found that in the core of massive neutron stars, neutron star matter includes rich particle species, such as antikaons, baryon octet, and △ quartet. In the presence of △ resonances and K^- condensation, the EOS becomes softer and results in smaller maximum mass stars. Furthermore the impact of antikaon condensations, hyperons, and △ resonances on direct Urca process with nucleons is also discussed briefly.     

基于眼模型的折/衍混合眼底相机设计

本文应用二元衍射光学理论,设计了一个基于Gullstrand-Le Grand眼光学模型的折/衍混合免散瞳手持式数字眼底相机。该相机的视场角28°,摄影系统由五片透镜构成,其中包含一个二元面,在综合考虑人眼本身和外部系统的像差后,实现了全视场200万像素的高清晰成像。而且,具有较大调焦能力,对-10D至7D屈光度人眼普遍适用。结果显示,该系统成像分辨率高于120lp/mm,场曲值小于0.75mm,畸变仅为7.0%。同时,衍射光学元件的引入,有效地简化了系统,减小了重量和体积。     

Neutrino Emission and Cooling of Dark-Matter-Admixed Neutron Stars

The GW170817 binary neutron star merger event in 2017 has raised great interest in the theoretical research f neutron stars. The structure and cooling properties of dark-matter-admixed neutron stars are studied here using relativistic mean field theory and cooling theories. The non-self-annihilating dark matter(DM) component is assumed to be ideal fermions, among which the weak interaction is considered. The results show that pulsars J1614-2230, J0348+0432 and EXO 0748-676 may all contain DM with the particle mass of 0.2–0.4 GeV. However,it is found that the effect of DM on neutron star cooling is complicated. Light DM particles favor the fast cooling of neutron stars, and the case is converse for middle massive DM. However, high massive DM particles, around1.0 GeV, make the low mass(around solar mass) neutron star still undergo direct Urca process of nucleons at the core, which leads the DM-admixed stars cool much more quickly than the normal neutron star, and cannot support the direct Urca process with a mass lower than 1.1 times solar mass. Thus, we may conjecture that if small(around solar mass) and super cold(at least surface temperature 5–10 times lower than that of the usual observed data) pulsars are observed, then the star may contain fermionic DM with weak self-interaction.