光栅最小偏向角法测量汞灯谱线波长的理论和实验验证

通过理论推导,给出了最小偏向角的表达式,测量得到最小偏向角的具体数值.实验结果表明,用最小偏向角法测量的波长较对称法更准确,另外,光栅常数也是影响实验误差的原因.     

最小偏向角的测量修正

从最小偏向角的特性入手，推导出了最小偏向角的测量修正公式，并在实验中进行了验证，从而提高了测量精度。     

最大偏向角法测光栅常量

结合光栅衍射实验中±1级衍射光随光栅片转动而分别向左右移动到某一位置消失的具体现象,在光栅实验中提出了“最大偏向角”的概念,并给出了通过测量最大偏向角来计算光栅常量的方法.     

模拟实验研究最小偏向角的规律

用分光计测量三棱镜折射率是一个间接测量实验,通过测量三棱镜的顶角和最小偏向角来计算获得折射率．本文通过编译程序模拟实验,描绘出偏向角随入射角、折射率变化的规律,进一步研究了最小偏向角与折射率间的对应关系．     

折射法检测透明液体浓度的研究

本文介绍一种测量透明液体浓度的方法，其基本原理是依据最小偏向角法，将溶液盛入空心三棱镜，测量光束沿最小偏向角的变化，拟合出液体浓度与角度变化的函数，实现浓度的测定。在该系统中，采用ＣＣＤ为接收器件，在很大范围内保证了不大于３％的测量精度。     

临界角法测三棱镜折射率

应用分光计测量三棱镜折射率，最常用的方法就是熟知的最小偏向角法，还有掠人射法[1]与等顶角入射法[3]．本文介绍临界法如下．按图示光路，由折射定律n棱镜折射率．i’全反射临界冷，为对应的偏向角．从几何关系可得若能求出r与、A的关系，就能测量、A计算出折射测量方法先按最小偏向法找到最小偏向角，将载物台继续朝原方向转动，边转动边观察狭缝像的移动及光强的变化，可以发现光强是愈来愈弱，狭缝像变得弥散，当望远镜的光轴与棱镜的AC面平行时，记录下左右游标读数，取下棱镜测入射光位置，可得偏向角，按常用方法测A。在一次测量…     

测定三棱镜折射率实验中要注意的问题

测定三棱镜折射率实验中要注意的问题卢勇（台州师专物理系３１７０００）一、问题的提出在分光计上测定三棱镜折射率，最关键的问题是准确测量最小偏向角δ０和折射角α，然后根据公式计算折折射率ｎ．但是学生在测量最小偏向角δ０时，往往出现较大的误差．对此作如下讨...     

测量晶体红外折射率的一种简便方法

一、引 言 非线性光学晶体在可见和近红外波段的折射率数据对于设计倍频、光参量振荡等器件来说是必不可少的.晶体在近红外波段折射率的测量通常采用测量晶体棱镜最小偏向角的方法.这需要采用一台反射式红外分光计[1],或者采用阿贝自准直棱镜自动调节最小偏向角的方法[2],用以克服不能用眼睛直接寻找红外光束最小偏向角的困难.但这两种方法都必须设计一套红外光的测量装置,光学系统比较复杂.我们提出了一种使用通常透射式测角仪测量晶体红外折射率的简便方法——最小偏向角和固定入射角相结合的方法.它既克服了不能用眼晴直接寻找最小偏向角…     

光栅条纹最小偏向角的实验研究

本文讨论了斜入射时光栅条纹偏向角存在最小值的实验观察现象及相关原理,提出了利用最小偏向角测量光波波长和光栅常数的方法,并在实验中对最小偏向角法和垂直入射法进行了分析比较.     

棱镜玻璃折射率的测定

本文介绍了一种高精度测量玻璃折射率的任意偏向角法，主要说明了该方法的实验原理、测量方法及理论误差分析。     

模拟实验研究最小偏向角的规律

本文通过编译程序模拟实验,描绘出偏向角随入射角、折射率变化的规律,进一步研究了最小偏向角与折射率间的对应关系。     

光束通过三棱镜的偏折情况再探讨

针对本科教学中学生关于三棱镜对光束偏折情况提出的疑惑,对光束通过三棱镜的多种偏折情况进行了详细分析,讨论了入射角、折射率、棱镜顶角对出射光线偏折方向的影响,给出了三棱镜的顶角和折射率的取值范围以及入射角的取值范围对光线是否能从出射边界射出,以及出射光线的偏折方向的影响,进一步讨论了光束的偏向角与三棱镜各参数之间的关系,给出了确定最小偏向角的简单方法.     

基于反馈式可定位云台控制系统设计与实现

摘要：针对原值监测对样品应具备准确定位监测及信息可控的要求,在云台中建立了偏转角度检测装置,采集云台偏转角度脉冲信息并反馈到解码器中,对脉冲信号通过建立偏转角度计算公式处理云台偏转角度信息,并反馈给上位机,从而在上位机操作台、解码器、云台三者间形成了反馈式可定位云台控制系统。实践表明,通过这种反馈式偏转角数据的引入,上位机随时根据下位机反馈的云台偏转角数据实时监控云台工作状态,实现操作台对云台的精确控制,从而提高云台的易操作性和智能化水平。     

Light’s bending angle due to black holes: from the photon sphere to infinity

The bending angle of light is a central quantity in the theory of gravitational lensing. We develop an analytical perturbation framework for calculating the bending angle of light rays lensed by a Schwarzschild black hole. Using a perturbation parameter given in terms of the gravitational radius of the black hole and the light ray’s impact parameter, we determine an invariant series for the strong-deflection bending angle that extends beyond the standard logarithmic deflection term used in the literature. In the process, we discovered an improvement to the standard logarithmic deflection term. Our perturbation framework is also used to derive as a consistency check, the recently found weak deflection bending angle series. We also reformulate the latter series in terms of a more natural invariant perturbation parameter, one that smoothly transitions between the weak and strong deflection series. We then compare our invariant strong deflection bending-angle series with the numerically integrated exact formal bending angle expression, and find less than 1% discrepancy for light rays as far out as twice the critical impact parameter. The paper concludes by showing that the strong and weak deflection bending angle series together provide an approximation that is within 1% of the exact bending angle value for light rays traversing anywhere between the photon sphere and infinity.     

Weak deflection angle of extended uncertainty principle black holes

We discuss the effects of quantum fluctuations spewed by a black hole on its deflection angle.The GaussBonnet theorem(GBT)is exploited with quantum corrections through the extended uncertainty principle(EUP),and the corresponding deflection angle is obtained.Moreover,we have attempted to broaden the scope of our work by subsuming the effects of plasma medium on the deflection angle.To demonstrate the degree of difference,the acquired results are compared with the prevailing findings.     

Study of the Deflection Angle and Shadow of Black Hole Solutions in Non-Plasma and Plasma Mediums Under the Effect of Einstein–Gauss–Bonnet Gravity

In this paper, the Gibbons and Werner technique is used to calculate the weak deflection angle for the black hole solution under the effects of Einstein–Gauss–Bonnet gravity. The Gauss–Bonnet theorem in the limits of weak field is used to evaluate the Gaussian optical curvature in order to obtain the results. The visual effects of the deflection angle on the impact parameter is also looked at and the smallest radius in the non-plasma/plasma medium. Moreover, in order to check the consistency of the results concerning the weak deflection angle, the Keeton and Petters approach is applied to study the deflection angle, which is the expansion of series with a single mass variable, which can be directly addressed by using the post–post Newtonian framework. Furthermore, the deflection angle and shadow under the influence of the plasma is examined by using the motion of particle in a non-magnetized plasma and pressure-free plasma medium as described by the new ray-tracing algorithm. It is shown that plasma as well as Einstein–Gauss-Bonnet gravity corrections are affected by shadows.     

二维光束扫描镜的非线性畸变

本文通过坐标变换导出了一种二维光束扫描系统的光束表达式.利用该表达式对扫描振镜的非线性畸变作了讨论.指出,这种畸变只在X镜的扫描方向上发生,而畸变的程度与Y镜的偏转角有关.     

Letter: Solar Gravitational Deflection of a Graviton

The solar gravitational deflection angle of a graviton is calculated through the scattering cross section of the graviton by the sun and shown to be equal to the light deflection angle as calculated from the null geodesic equation of general relativity.     

Gravitational Lensing of STU Black Holes

In this paper we study gravitational lensing by STU black holes. We considered extremal limit of two special cases of zero-charged and one-charged black holes, and obtain the deflection angle. We find that the black hole charge increases the deflection angle.