"伏安法"测电阻中的几个问题

“伏安法”测电阻,包含了欧姆定律和电路连接等知识,有利于培养学生理论联系实际,实事求是地分析问题、解决问题的能力,同时是以后有关电学实验的基础。本文就其中的几个问题加以分析。     

差值法测电阻实验设计一例

伏安法测电阻是高中电学的一个重要实验，也是欧姆定律的一个实际应用．在传统的两种接线方法中，由于电流表和电压表接人电路时，不可视为理想情形(RA=0，Rv=∞)，从而改变了电路的结构，因而不能同时准确测出Rx两端电压及流过的电流，不可避免地出现系统误差．在此，笔者设计一种新的测量电路，来消除系统误差，对伏安法测电阻的实验做些改进．     

用替代法消除伏安法测电阻的系统误差

分析了伏安法测电阻的不足,介绍了采用替代法,在保证电路不变的情况下,用标准电阻箱夫代电压表、电流表或被测电阻,从而直接得出Ｒｖ,Ｒ∧,Ｒ,再求出Ｒ真。     

对伏安法测电阻的研究

对伏安法测电阻的研究魏诺（西安建筑科技大学７１００５５）伏安法测电阻通常存在两点不足：一是不考虑电表内阻误差的影响，二是按等精度测量进行数据处理．实际上，用伏安法测电阻时，在电表量程内由小到大选取不同值进行多次测量属于不等精度测量；而电表内阻的误差对...     

从典型实验中拓展学生的思路

通过物理实验中的一些典型内容来拓展学生的思路，从而使学生认识到基础知识到基础知识的重要性，通过教学上的改革来培养和增进学生的创造能力。     

改进测电阻方法

1测量电阻器的电阻Rx 常用电流表的内接法或外接法伏安法测Rx.由于忽略RV、RA的影响,实验测量存在系统误差.减小误差测法如图1、图2所示.     

用伏安法测电阻实验中电路的选择

在“用伏安法测电阻”实验中，要么采用电流表内接电路（图1），要么采用电流表外接电路（图2）．因为电流表的内阻RA并不为零，电压表的内阻RV也不是无限大，无论采用哪一种电路进行测量，系统误差总是不可避免的，这就是所谓的“方法误差”．当待测电阻阻值R满足RWR＾时，用内接法测量所带来的误差可忽略不计．”当待测电阻阻值R满足RV＞＞R时，用外接法测量所带来的误差可忽略不计．但在一般阻值的情况下，应该选用何种电路来进行测量才能使误差较小呢？本文将从误差分析入手来进行讨论，最后得出一个联接方式选择的判断方法．1内接…     

逃逸函数算法及其在光学设计中的应用

用阻尼最小二乘法进行光学系统的优化 ,得到的结果往往是评价函数在结构变量空间的一个局部极小值。日本东京工艺大学的一色教授提出了能够跳出此局部极小值继续寻找其它结果的逃逸函数全局优化算法 ,该算法的运行由多个不加或加入逃逸函数的阻尼最小二乘法局部优化组成。描述了逃逸函数的基本原理 ,给出了北京理工大学研制的GOLD软件在加入了这种算法后对光学系统进行全局优化的设计实例。实验证明了逃逸函数算法是提高光学设计效率和质量的一种有效工具。     

探月飞行器效能评估研究与实践

航天器飞行效能评估是整器级测试验证以及在轨飞行结果评价中不可或缺的重要环节,针对我国探月三期月地高速再入返回飞行试验,提出了一种基于任务剖面的航天器飞行效能评估方案;提取7个任务剖面、17个约束条件,建立面向月地再入返回过程的指标评估体系;通过定量、定性指标量化计算、权重系数层次分析法计算各任务剖面的能力度量值,解决了系统目标完成能力不易定量描述的难题,实现了对月地转移段、大气层外自由飞行段、再入段、跃出段等过程自主飞行能力的科学定量评估,对后续月球无人采样返回、火星探测等探测器系统的效能评估具有一定参考意义;该方法已应用于月地高速再入返回飞行器系统。     

Environmental test of the BGO calorimeterfor DArk Matter Particle Explorer

DArk Matter Particle Explorer (DAMPE) is the first Chinese astronomical satellite, successfully launched on Dec. 17 2015. As the most important payload of DAMPE, the BGO calorimeter contains 308 bismuth germanate crystals, with 616 photomultiplier tubes, one coupled to each end of every crystal. Environmental tests have been carried out to explore the environmental adaptability of the flight model of the BGO calorimeter. In this work we report the results of the vibration tests. During the vibration tests, no visible damage occurred in the mechanical assembly. After random or sinusoidal vibrations, the change of the first order natural frequency of BGO calorimeter during the modal surveys is less than 5%. The shift ratio of Most Probable Value of MIPs changes in cosmic-ray tests are shown, the mean value of which is about -4%. The comparison of results of cosmic-ray tests before and after the vibration shows no significant change in the performance of the BGO calorimeter. All these results suggest that the calorimeter and its structure have passed through the environment tests successfully.     

Search for Sub-Solar Mass Binaries with Einstein Telescope and Cosmic Explorer

A possible detection of sub-solar mass ultra-compact objects would lead to new perspectives on the existence of black holes that are not of astrophysical origin and/or pertain to formation scenarios of exotic ultra-compact objects. Both possibilities open new perspectives for better understanding of our universe. In this work, we investigate the significance of detection of sub-solar mass binaries with components mass in the range: 10−2M⊙ up to 1M⊙, within the expected sensitivity of the ground-based gravitational waves detectors of third generation, viz., the Einstein Telescope (ET) and the Cosmic Explorer (CE). Assuming a minimum of amplitude signal-to-noise ratio for detection, viz., ρ=8, we find that the maximum horizon distances for an ultra-compact binary system with components mass 10−2M⊙ and 1M⊙ are 40 Mpc and 1.89 Gpc, respectively, for ET, and 125 Mpc and 5.8 Gpc, respectively, for CE. Other cases are also presented in the text. We derive the merger rate and discuss consequences on the abundances of primordial black hole (PBH), fPBH. Considering the entire mass range [10−2–1]M⊙, we find fPBH<0.70 (<0.06) for ET (CE), respectively.     

Dark Matter Particle Explorer observations of high-energy cosmic ray electrons plus positrons and their physical implications

The DArk Matter Particle Explorer(DAMPE) is a satellite-borne, high-energy particle and γ-ray detector, which is dedicated to indirectly detecting particle dark matter and studying high-energy astrophysics. The first results about precise measurement of the cosmic ray electron plus positron spectrum between 25 Ge V and 4.6 Te V were published recently. The DAMPE spectrum reveals an interesting spectral softening arount 0.9 Te V and a tentative peak around 1.4 Te V. These results have inspired extensive discussion. The detector of DAMPE, the data analysis, and the first results are introduced. In particular, the physical interpretations of the DAMPE data are reviewed.     

Impacts of gravitational-wave standard siren observations from Einstein Telescope and Cosmic Explorer on weighing neutrinos in interacting dark energy models

Multi-messenger gravitational wave (GW) observation for binary neutron star merger events could provide a rather useful tool to explore the evolution of the Universe. In particular, for the third-generation GW detectors, i.e. the Einstein Telescope (ET) and the Cosmic Explorer (CE), proposed to be built in Europe and the U.S., respectively, lots of GW standard sirens with known redshifts could be obtained, which would exert great impacts on the cosmological parameter estimation. The total neutrino mass could be measured by cosmological observations, but such a measurement is model-dependent and currently only gives an upper limit. In this work, we wish to investigate whether the GW standard sirens observed by ET and CE could help improve the constraint on the neutrino mass, in particular in the interacting dark energy (IDE) models. We find that the GW standard siren observations from ET and CE can only slightly improve the constraint on the neutrino mass in the IDE models, compared to the current limit. The improvements in the IDE models are weaker than those in the standard cosmological model. Although the limit on neutrino mass can only be slightly updated, the constraints on other cosmological parameters can be significantly improved by using the GW observations.