弹簧摆在匀强磁场中的运动分析

针对带有电荷的弹簧摆施加在竖直方向的匀强磁场的背景下,通过牛顿力学的方法得到了其运动学方程,从而发现其摆动平面在不停的进行旋转.同时按照初始条件的不同,将其在水平方向上的运动学方程化简为不同的曲线方程,进而得到了其运动的轨迹特征.     

带电粒子在匀强电场和匀强磁场中运动规律的研究

先通过牛顿运动第二定律推出带电粒子在匀强电场和匀强磁场中运动的微分方程组,再利用数学软件Maple解出方程组的解析解,对解析解的进一步分析证明带电粒子在运动过程中加速度大小不变,最后通过Maple对解析解进行数值模拟,得到了带电粒子在复合场中的5种常见的运动轨迹.     

匀强磁场产生装置的设计

阐述了亥姆霍兹线圈轴线上磁感应强度高阶导数的奇特性质,提出利用共轴四线圈组产生均匀磁场的设想,并通过模拟共轴四线圈组磁场的轴线分布及空间分布,展现了共轴四线圈组的优越之处.     

匀强磁场中任意刚性导线的动生电动势

匀强磁场中导体做切割磁感线运动而产生的动生电动势公式E =B L v只适用于特定情形. 如何将其 推广是一个热点话题. 本文以导线微元动生电动势的一般公式和刚体运动特征为起点, 将动生电动势公式推广到 直导线的任意运动以及任意形状的刚性导线的任意运动情形, 得到了3条结论, 并对它们进行了证明     

带电粒子在矩形边界匀强磁场中经过某一点的问题

从2019年高考全国卷物理带电粒子在匀强磁场中的偏转问题出发,结合在平时教学中遇到的带电粒子在矩形边界磁场中经过某一点的问题,提出了从角度关系解决这一问题的思路与方法,以期辅助学生简洁快速地解决该类问题.     

人教版《带电粒子在匀强磁场中的运动》教学设计

在新课程要求下,如何在具体的教学中落实知识与技能、过程与方法、情感态度与价值观三维目标,是广大高中教师需要深入思考和研究的问题．本文以人教版《带电粒子在匀强磁场中的运动》的教学为例,尝试将问题探究式引入课堂教学,促进课程三维目标实现．     

3个共轴圆线圈形成的匀强磁场

分析了3个共轴圆线圈形成磁场的均匀性，得到了3个共轴圆线圈形成匀强磁场的条件，并且通过数值计算，全面展示3个共轴圆线圈磁场的均匀性．只要合理配置3个共轴圆线圈的大小、线圈中的电流强度和线圈之间的距离，3个共轴圆线圈的磁场在强度和均匀性方面都优于亥姆霍兹线圈的磁场。     

匀强磁场对刚性载流线圈磁力矩公式的一般推导

利用矢量代数和矢量场论的有关结果严谨地推证了匀强磁场中载流线圈所受合磁力矩表达式。     

试议加正交匀强磁场后,对做平抛运动的带电小球飞行落地时间的影响

很多参考书、复习资料上都有求加正交匀强磁场后,对做平抛运动的带电小球落地时间影响的题目,但求解都没有详细过程,只是在竖直方向上讨论一下平均加速度直接得出结果,学生总觉得雾里看花,模糊不清.其实不妨从运动的合成与分解着手,采用图像法作一定性分析.     

斯特恩——盖拉赫实验中非匀强磁场的等效和钾原子的速度分布

近年来,斯特恩——盖拉赫实验装置在我国研制成功,填补了高校近代物理实验的一个空白。这一实验在原子物理和量子力学中只作原理性的简单介绍。在此,我们就该实验装置的核心部件——非匀强磁场的等效和实验中关于钾原子束的速度分布及其它对偏移束流强度的分佑影响等作较详尽的论述,以充实历史上这一著名实验的教学内容。一、双导线等效磁场——非匀强磁场图1为斯特恩——盖拉赫实验装置中用     

Comparison between the single-bubble sonoluminescences in sulfuric acid and in water

Single-bubble sonoluminescence (SBSL) is achieved with strong stability in sulfuric acid solutions. Bubble dynamics and the SBSL spectroscopy in the sulfuric acid solutions with different concentrations are studied with phase-locked integral stroboscopic photography method and a spectrograph, respectively. The experimental results are compared with those in water. The SBSL in sulfuric acid is brighter than that in water. One of the most important reasons for that is the larger viscosity of sulfuric acid, which results in the larger ambient radius and thus the more contents of luminous material inside the bubble. However, sonoluminescence bubble’s collapse in sulfuric acid is less violent than that in water, and the corresponding blackbody radiation temperature of the SBSL in sulfuric acid is lower than that in water. Supported by the National Natural Science Foundation of China (Grant Nos. 10434070 and 10704037) and the Ministry of Education Priorities Project of China (Grant No. 103078)     

Multi-bubble motion behavior of uniform magnetic field based on phase field model

Aiming at the interaction and coalescence of bubbles in gas–liquid two-phase flow, a multi-field coupling model was established to simulate deformation and dynamics of multi-bubble in gas–liquid two-phase flow by coupling magnetic field, phase field, continuity equation, and momentum equation. Using the phase field method to capture the interface of two phases, the geometric deformation and dynamics of a pair of coaxial vertical rising bubbles under the applied uniform magnetic field in the vertical direction were investigated. The correctness of results is verified by mass conservation method and the comparison of the existing results. The results show that the applied uniform magnetic field can effectively shorten the distance between the leading bubble and the trailing bubble, the time of bubbles coalescence, and increase the velocity of bubbles coalescence. Within a certain range, as the intensity of the applied uniform magnetic field increases, the velocity of bubbles coalescence is proportional to the intensity of the magnetic field, and the time of bubbles coalescence is inversely proportional to the intensity of the magnetic field.     

亥姆霍兹线圈磁场的探究

定量计算了亥姆霍兹线圈空间磁场的分布,并用Mathmatic进行空间模拟,形象地描述了亥姆霍兹线圈的空间磁场分布,同时就其均匀性与三线圈和载荷旋转圆盘的磁场进行了对比讨论.     

Effect of change in large and fast solar wind dynamic pressure on geosynchronous magnetic field

We present a comparison of changes in large and sharp solar wind dynamic pressure, observed by several spacecraft, with fast disturbances in the magnetospheric magnetic field, measured by the geosynchronous satellites. More than 260 changes in solar wind pressure during the period 1996--2003 are selected for this study. Large statistics show that an increase (a decrease) in dynamic pressure always results in an increase (a decrease) in the magnitude of geosynchronous magnetic field. The amplitude of response to the geomagnetic field strongly depends on the location of observer relative to the noon meridian, the value of pressure before disturbance, and the change in amplitude of pressure.     

导体对磁场的屏蔽作用分析

分析了导体球壳对静磁场和对交变磁场的屏蔽作用,讨论了影响导体球壳对静磁场和对交变磁场的屏蔽作用的因素.     

Microscopic calculation of the magnetic field of neutron stars

Based on the Dirac equation describing an electron moving in a uniform and cylindrically symmetric magnetic field which may be the result of the self-consistent mean field of the electrons themselves in a neutron star, we have obtained the eigen solutions and the orbital magnetic moments of electrons in which each eigen orbital can be calculated. From the eigen energy spectrum we find that the lowest energy level is the highly degenerate orbitals with the quantum numbers pZ=0, n=0, and m≥0. At the ground state, the electrons fill the lowest eigen states to form many Landau magnetic cells and each cell is a circular disk with the radius λfree and the thickness λe, where λfree is the electron mean free path determined by Coulomb cross section and electron density and λe is the electron Compton wavelength. The magnetic moment of each cell and the number of cells in the neutron star are calculated, from which the total magnetic moment and magnetic field of the neutron star can be calculated. The results are compared with the observational data and the agreement is reasonable.     

亥姆霍兹线圈磁场均匀范围的研究

推导了双环电流磁感应强度在直角坐标系中的解析式,将公式无量纲化,通过第一类和第二类完全椭圆积分计算场强的两个分量,从而计算合场强,画出亥姆霍兹线圈内外磁感应强度合场强曲面和三维均匀区域,发现磁场的均匀区域是"八爪"形状,并与双环电流不同距离的场强和均匀范围进行了比较.     

Microscopic calculation of the magnetic field of neutron stars

Based on the Dirac equation describing an electron moving in a uniform and cylindrically symmetric magnetic field which may be the result of the self-consistent mean field of the electrons themselves in a neutron star, we have obtained the eigen solutions and the orbital magnetic moments of electrons in which each eigen orbital can be calculated. From the eigen energy spectrum we find that the lowest energy level is the highly degenerate orbitals with the quantum numbers pz = 0, n = 0, and m ≥0. At the ground state, the electrons fill the lowest eigen states to form many Landau magnetic cells and each cell is a circular disk with the radius λfree and the thickness λe, where λfree is the electron mean free path determined by Coulomb cross section and electron density and λe is the electron Compton wavelength. The magnetic moment of each cell and the number of cells in the neutron star are calculated, from which the total magnetic moment and magnetic field of the neutron star can be calculated. The results are compared with the observational data and the agreement is reasonable.