近场光学显微技术

本文在介绍近场光学显微镜原理的基础上，对近场光学显微技术进行了一定深度的探讨，并着重研究了纳米级探针的制作和纳米级样品与探针间距的控制这两个近场光学显微技术中的关键问题，说明了近场光学显微探针的工作方式，阐述了近场光学成像的衬度类型，介绍了近场光学显微技术在多个领域的应用。在参考大量国内外最新研究成果的基础上，提出了一些个人的见解。     

非探针近场光学显微镜的成像实现

介绍一种非探针近场光学显微镜，并对它的图像实现过程及处理方法进行了讨论。该装置以阿达玛变换成像理论为基础，用纳米多孔编码板代替光纤探针获得了较高的光学信噪比。成像研究表明，该装置可对近场衰逝波分量进行有效探测并能实现超衍射极限成像，为近场光学探测研究提供了一种新的思路。     

近场扫描光学显微镜和近场光谱学的进展

在简要评介近场扫描光学显微镜的工作原理和有关技术问题的基础上，着重介绍了近场光谱学的最新发展，并讨论了对近场光谱结果的分析问题。     

纳变尺度的光学成像与纳米光谱：近场光学与近场光学显微镜的进展

近场光学是指当光探测器及探测器一样品间距均小于辐射波长条件下的光学现象，利用近场光学扫描显微镜和近场光谱仪，不但能够以突破衍射极限的超高分辨率在纳米尺度实现光学成像，而且还可获得纳米微区的光谱信息，文章介绍近场光学的原理及其在凝聚态物理领域中的应用与进展，并给出了我们的初步结果。     

纳米尺度的光学成像与纳米光谱———近场光学与近场光学显微镜的进展

近场光学是指当光探测器及探测器－样品间距均小于辐射波长条件下的光学现象．利用近场光学扫描显微镜和近场光谱仪，不但能够以突破衍射极限的超高分辨率在纳米尺度实现光学成像，而且还可获得纳米微区的光谱信息．文章介绍近场光学的原理及其在凝聚态物理领域中的应用与进展，并给出了我们的初步结果     

纳米光学和生物单分子探测

纳米光学技术展示了纳米级探测本领，同时生物单分子探测所需要分辨尺度也是纳米数量级的，因此在生物单分子探测过程中，纳米光学发挥了巨大的作用．文章介绍了与生物单分子探测技术相关的纳米光学技术，包括量子近场光学探针技术、近场光学成像技术(包括扫描近场光学显微术及全内反射荧光显微术)和激光光钳测控技术及它们在生物单分子探测上的进展，从而在染色、成像、测控三个方面展示了纳米光学技术在生物方面的应用，并对其未来的发展方向进行了展望．     

基于纳米孔径激光器的近场光存储的最新发展

近几年发展起来的近场光学原理和方法为实现超高密度光学数据存储开辟了新的技术途径。基于近扬光学方法的最小信息记录单元尺寸突破了经典光学分辨率的衍射极限 ,理论存储密度高达 1 0 0 0Gb/平方英寸 ,受到了研究人员和工业界的广泛关注。着重介绍了用于近场光学存储的纳米孔径激光器的原理、结构、优点 ,对它的实现方法和发展状况作了详细的阐述 ,并对其在近场光存储领域未来的发展趋势进行了展望     

微波模拟近场光学显微镜实验

介绍了近场光学显微镜的基本原理，并利用微波代替可见光模拟了近场光学显微镜实验．     

近场光学在高密度存储中的应用

近场光学在高密度存储方面有着很大的潜力 ,使得近场光学存储近年来得到了广泛的关注。近场光学存储具有高密度大容量及可以利用许多已有相关技术等优点 ,预计近场光学存储密度能达到 7Gbit/ cm2 ;它还可以采用硬盘驱动器中的空气悬浮磁头技术和磁光存储中的技术等 ,使近场存储的研究和开发更加迅速。目前 ,近场光学存储主要有三种方案 :探针型方案、超分辨率近场结构、固体浸没透镜方案 ,这三种方案都是通过不同的方法缩小记录光斑来实现高密度的存储。介绍了近场光学存储的原理、研究现状及材料 ,并对三种近场存储方案的实现方法和发展概况作了详细的阐述 ,分析了这三种方案的优缺点     

近场光存储及其研究进展

本文从近场光学的超分辨原理出发详细介绍和分析了孔径探针型近场光存储技术，SIL透镜近场光存储技术和近场超分辨结构光盘存储技术等的基本原理、研究现状以及它们的优缺点及存在的问题。     

模型参数对奇异星性质的影响

用有效质量口袋模型描述奇异夸克物质,研究了耦合常数和口袋常数的选取对奇异夸克物质的状态方程及奇异星性质的影响.结果表明,随着耦合常数和口袋常数的增大,奇异夸克物质的状态方程变软,相应的奇异星的引力质量和对应的半径均变小.当耦合常数从0.5增大到2.0时,奇异星的质量从1.43M_⊙(M_⊙=1.99×10³⁰ kg)减小到1.25M_⊙,相应的半径由8.3 km减小到7.7 km;当口袋常数B^1/4由160 MeV增大到175 MeV时,奇异星的质量和半径分别由1.47M_⊙和8.6 km减小到1.22M_⊙和7.4 km.这说明奇异夸克物质及奇异星的性质明显依赖于模型参数的取值. 关键词： 模型参数 奇异星 状态方程 质量-半径关系     

Cooling Curve of Strange Star in Strong Magnetic Field

In this paper, firstly, we investigate the neutrino emissivity from quark Urca process in strong magnetic field. Then, we discuss the heat capacity of strange stars in strong magnetic field. Finally, we give the cooling curve in strong magnetic field. In order to make a comparison, we also give the corresponding cooling curve in the case of null magnetic field. It turns out that strange stars cool faster in strong magnetic field than that without magnetic field.     

准粒子描述下奇异夸克物质自洽热力学及对奇异星物态的影响

考虑夸克粒子间相互作用,研究了在准粒子近似下奇异夸克物质系统的热力学,发现由于热力学自洽的要求,需要在热力学势中额外增加一项.利用这一等效热力学讨论奇异夸克物质的物态方程及声速,得到了一个“软化”的物态,这与质量–密度相关模型是一致的.但准粒子描述模型能够显示介质效应对强相互作用耦合常数的依赖.     

Anisotropic strange quark star in Finch-Skea geometry and its maximum mass for non-zero strange quark mass (ms ≠ 0)

A class of relativistic astrophysical compact objects is analyzed in the modified Finch-Skea geometry described by the MIT bag model equation of state of interior matter, \begin{document}$ p=\dfrac{1}{3}\left(\rho-4B\right) $\end{document}, where B is known as the bag constant. B plays an important role in determining the physical features and structure of strange stars. We consider the finite mass of the strange quark (\begin{document}$ m_{s} \neq 0 $\end{document}) and study its effects on the stability of quark matter inside a star. We note that the inclusion of strange quark mass affects the gross properties of the stellar configuration, such as maximum mass, surface red-shift, and the radius of strange quark stars. To apply our model physically, we consider three compact objects, namely, (i) VELA X-1, (ii) 4U 1820-30, and (iii) PSR J 1903+327, which are thought to be strange stars. The range of B is restricted from 57.55 to \begin{document}$B_{\rm stable}$\end{document} (\begin{document}$\rm MeV/fm^{3}$\end{document}), for which strange matter might be stable relative to iron (\begin{document}$^{56}{\rm Fe}$\end{document}). However, we also observe that metastable and unstable strange matter depend on B and \begin{document}$ m_{s} $\end{document}. All energy conditions hold well in this approach. Stability in terms of the Lagrangian perturbation of radial pressure is studied in this paper.     

Strange quark star and the parameter space of the quasi-particle model

The properties of strange quark stars are studied within the quasi-particle model. Taking into account chemical equilibrium and charge neutrality, the equation of state(EOS) of(2+ 1)-flavor quark matter is obtained. We illustrate the parameter spaces with constraints from two aspects: one is based on the astronomical results of PSR J0740+ 6620 and GW 170 817,and the other is based on the constraints proposed from the theoretical study of a compact star that the EOS must ensure the tidal deformability Λ_(1.4)=190_(-120)~(+390) and support a maximum mass above 1.97M_⊙. It is found that neither type of constraints can restrict the parameter space of the quasi-particle model in a reliable region and thus we conclude that the low mass compact star cannot be a strange quark star.     

高温近似下奇异夸克物质的体粘滞系数

在准粒子描述下,采用自洽的热力学方法,考虑奇异夸克物质(SQM?)的介质效应,计算了高温近似下奇异夸克物质的体粘滞系数.发现介质效应对奇异夸克物质的体粘滞系数有很大影响,这使得观测数据不再排除两味色超导相奇异星的存在.     

Cooling Curve of Strange Star in Strong Magnetic Field

In this paper, firstly, we investigate the neutrino emissivity from quark Urca process in strong magnetic field. Then, we discuss the heat capacity of strange stars in strong magnetic field. Finally, we give the cooling curve in strong magnetic field. In order to make a comparison, we also give the corresponding cooling curve in the case of null magnetic field. It turns out that strange stars cool faster in strong magnetic field than that without magnetic field.     

Radial oscillations of magnetized proto strange stars in temperature- and density-dependent quark mass model

We report on the study of the mass-radius (M–R) relation and the radial oscillations of magnetized proto strange stars. For the quark matter we have employed the very recent modification, the temperature- and density-dependent quark mass model of the well-known density-dependent quark mass model. We find that the effect of magnetic field, both on the maximum mass and radial frequencies, is rather small. Also a proto strange star, whether magnetized or otherwise, is more likely to evolve into a strange star rather than transform into a black hole.     

Effects of Density-Dependent Bag Constant and Strange Star Rotation

With the emphasis on the effects of the density-dependent bag constant and the rotation of strange star the limiting mass of strange star is calculated. The obtained results show that the limiting mass and the corresponding radius of strange star increase as the rotation frequency increases, and tend to be lowered when the density-dependent bag constant is considered.     

奇异星物理的新进展

奇异夸克物质被推测比核物质更稳定,奇异星可能存在。人们关于奇异星的研究已越来越深入。本文较详细地评述奇异星物理的研究进展,并特别强调奇异星和中子星的区别。