低介电常数超材料在反射型磁光隔离器中的应用

为设计厚度薄、层数少且具有良好工作性能的反射型磁光隔离器,在一维单缺陷磁光光子晶体中引入低介电常数超材料.利用传输矩阵法研究该光子晶体的克尔磁光效应,结果表明,采用低介电常数超材料制备层间阻抗差异较大的一维单缺陷磁光光子晶体,既易于在磁光介质层形成较强的局域场,获得接近45°的克尔旋转角,又可增强光的反射,获得较高的能量反射率.本研究为低介电常数超材料应用提供了新的可能.     

应用于光隔离器的一维磁光光子晶体结构探索

采用传输矩阵方法分析了一维磁光光子晶体.对不同结构参量下的磁光多层膜的光学性质进行了数值计算.得到了一种新颖实用的磁光多层膜结构,可用作实现光集成应用中的光隔离器的元件.典型磁光材料的厚度仅为2.13 μm,一维磁性光子晶体的总厚度仅为7.03 μm.     

反射型磁光多层膜隔离器工作稳定性的研究

与单纯的磁光晶体相比,由磁光介质与电介质周期性或准周期性排列构成的一维磁光光子晶 体能够显著增强磁光效应,可以用于实现小尺度的磁光隔离器,从而大大减小器件的尺寸. 给出更为一般的可用于求解斜入射情况下偏振光在各向异性介质中传播时的传输矩阵方法, 并用这种方法在波长为1053μm处,针对两种“三明治”型的反射磁光多层膜隔离器的 结构,具体讨论了器件应用时入射角度及工艺制作时膜层制备厚度对它们工作稳定性的影响 .发现中心磁光介质夹层较厚的结构具有膜层数目少、工作稳定性好的优点. 关键词： 光隔离器 磁光效应 一维光子晶体     

多缺陷结构的一维磁光多层膜隔离器

由磁光介质（M）和电介质（G）周期性排列构成的磁光光子晶体会出现很强的光 局域性，最近用它来实现磁光隔离器引起人们广泛的兴趣.给出了一种可用于计算 偏振光在各向异性介质传播问题的传输矩阵方法.并用该方法计算了对称多缺陷结构磁光多 层膜隔离器的光学性质，发现随着缺陷数目的增多，旋转角及透过率的频谱响应得到改善. 当缺陷增加到一定数目时，不需要额外的反射层即可实现反射型磁光隔离器的要求. 关键词： 光隔离器 磁光效应 多层膜 光子晶体     

大入射角一维磁光子晶体宽带光隔离器

采用4×4传输矩阵法研究了复合一维磁光子晶体隔离器的特性,当外加磁场与光路光轴方向夹角为19.95°时,用20.16μm的总厚度实现了中心波长附近3.1nm的宽带光隔离,当光线入射角为3.9°时,仍可实现1.06nm的宽带滤波,且其透射谱平坦性良好.该光隔离器可以同时满足隔离宽度、透射谱平坦性以及对光线入射角宽容性的要求,在实际运用中具有重要的实用价值.     

反射型磁光多层膜隔离器的频率响应及宽容性研究

通过传输矩阵法分析了材料介电常数的变化对于单缺陷结构的磁光多层膜隔离器性能的响，并提出了一种多缺陷结构的磁光多层膜结构.同单缺陷结构相比，多缺陷结构的旋转角的频谱响应带宽有很大增加，对于材料介电常数变化的宽容性得到了一个数量级的提高.同时这种多缺陷的结构对于膜层厚度的变化和入射角度也有很好的宽容性. 关键词： 光隔离器 磁光效应 一维光子晶体     

基于空气缺陷的光子晶体可调谐滤波器

采用传输矩阵法分别模拟了缺陷层厚度、入射角度和膜厚微扰的变化对含空气缺陷的一维光子晶体滤波特性的影响.研究表明:对于空气厚度可调结构,在考虑色散的情况下,空气厚度每增加2nm透射波长相应向长波方向移动约2nm,二者基本呈1∶1的线性关系;对于入射角度可调结构,与正入射相比较,入射角度从0°到89°变化时,其全角度禁带分别减小了105nm(TE模)、600nm(TM模),TM模禁带受角度的变化影响较大;入射角从0°分别变化到16.9°(TE模)、17.0°(TM模)时实现C波段的可调滤波.同一周期内,两种材料的模厚误差的相互弥补,能够实现小范围的膜厚扰动不敏感,缩小实际滤过峰值与理论值的偏差,可降低制备光子晶体的难度.     

含复合缺陷层的光子晶体的光学特性

运用传输矩阵法研究了在一维光子晶体中插入缺陷层的透光特性。在无缺陷层的一维光子晶体中能产生467~510 nm、1 279~1 715 nm两处明显的光子带隙。重点研究了插入缺陷层后,在1 279~1 715 nm的光子带隙中缺陷层厚度和入射角度大小分别与透射光谱变化的关系。研究发现：缺陷模的位置对入射角变化很敏感;出现缺陷模的数量和插入缺陷层的数量相同;一维光子晶体厚度的增大不会改变缺陷模的数量和位置,只改变透射峰的宽度和透射率。     

光子晶体四信道波分复用器的研究

提出了一种由2-D光子晶体构成的四信道波分复用系统。该系统包括利用光子晶体的线缺陷实现的波导部分和利用光子晶体微腔实现的频率选择部分。采用时域有限差分(FDTD)方法,研究了光在含点缺陷(即微腔)和线缺陷(即波导)的光子晶体中的传输特性,并给出了仿真结果。计算结果表明,该结构可以实现波长为λ=1550nm附近的四信道波分复用。     

含Co_6Ag_(94)三明治结构的光学和磁光性质EI北大核心CSCD

利用隧穿机制研究了含磁光金属Co6Ag94的三明治结构(磁光金属嵌入两个磁光光子晶体中)的透射性质和磁光法拉第旋转效应。在含磁光金属的三明治结构中,分别研究了双透射峰和单透射峰两种情况。研究结果表明,无论是双透射峰还是单透射峰情况,局域在磁光金属和磁光光子晶体界面上的电磁场,都能够同时增强磁光金属的透射和磁光法拉第旋转效应。另外,分析了磁光金属Co6Ag94存在增益时该三明治结构法拉第旋转角达到-45°的情况,此性质为设计小型化的磁光隔离器件提供了理论依据。     

关于"太阳在银河系中所受引力与到银心距离r的关系"的讨论

讨论了银道面内的引力场强分布和太阳在银河系中所受引力与到银心距离r的关系，指出引力场强g并不是与r的平方成反比，这是由于银河系的大小和形状不能忽略造成的．强调了万有引力定律的适用条件．     

On the predictability of the positions of the convergence zones in the ocean

The disagreement between the experimental and calculated positions of the first convergence zone are known from many publications. The most probable cause for such a disagreement, namely, the incorrect specification of the input data for the calculations, is considered. The lack of simultaneity between the hydrological surveys of the region and the acoustic experiments is emphasized. The experimental data obtained by the author in five ocean regions are presented. These data characterize the diurnal variability of the distance from the source to the nearest boundary of the convergence zone. The relations proposed by different researchers for calculating the sound speed from the temperature, salinity, and hydrostatic pressure are analyzed. It is shown that these relations lead to a substantial difference in the estimated depth dependence of the hydrostatic gradient of the sound speed. The position of the first convergence zone is calculated for the propagation conditions determined by vertical temperature and salinity profiles with the subsequent recalculation of these profiles into sound speed profiles by using eight different formulas known from the literature. It is shown that different formulas lead to different values of the distance to the first zone; this difference is substantially greater than that between the calculations and experiment. The necessity of improving the recalculation relations in view of the experimental data on sound propagation in natural oceanic waveguides, including the data on the actual positions of the convergence zones, is emphasized.     

On the calculation of the bremsstrahlung in the region of the plasma frequency

On the basis of the classical theory of radiation produced in incomplete Coulomb interaction, a formula is derived for the coefficient of the bremsstrahlung of fully ionized plasma. In the region of rectilinear approximation a comparison is made with the results of the quantum formula derived from the Born approximation. Furthermore, the influence of dispersion upon the emission coefficient is taken into account; some relations for the region of dispersion are given.     

Dependence of the Intensity of the Spectral Lines and the Composition of the Sample and the Plasma Parameters of the Unipolar Arc

The investigation was made of the dependence of the intensity of Tl, Ga, Mo, Mg, Mn, Sn, Bi, Ni, Zn, Pt and Au spectral lines and the plasma parameters (temperature T, electron concentration n_e, degree of 6 ionnization α) from concentration of lithium additive.     

Extracting the wavefunction of the LSP at the LHC

We consider associated production of squarks and gluinos with the lightest supersymmetric particle (LSP), or states nearly degenerate in mass with it. Though sub-dominant to pair production of color SU(3)-charged superpartners, these processes are directly sensitive to the wavefunction composition of the lightest neutralinos. Exploiting event-shape variables - including some introduced here for the first time - we are able to identify the composition of the LSP by selecting events involving a single high-pT jet recoiling against missing transverse energy. We illustrate the proposed technique on a set of benchmark cases and propose methods for applying these results in more realistic experimental environments.     

Set the controls for the heart of the Sun

In this paper we describe experiments conducted with high-power lasers that are attempting to replicate, for a very short time and in miniature, conditions found in the Sun. Experiments to date have reached conditions in the outer part of the Sun. To reach the Sun's centre requires compression of material to very much greater than solid density and heating to over ten million degrees. To achieve this, a new class of experiments and a new generation of high-power lasers are required.     

On the Question of the Source of the Apokamp

Technical Physics - The object of this work is the apokamp—a new type of plasma jet, which is formed from a bright offshoot emerging at the bending point of a channel of a high-voltage...