微扰法计算中等强磁场中氢原子的能级

本文在考虑氢原子轨道运动磁矩与磁场之间、自旋磁矩与磁场之间和感生磁矩与外磁场之间的相互作用的基础上,根据角动量和球谐函数的性质,应用简并态微扰方法研究了在中等强磁场中氢原子的能级,给出了计算中等强磁场中氢原子的一级近似能级的方法,具体计算了23.5126≤B≤1.881728×10~4T范围内氢原子n=2的各能级的数值,结果与有关文献给出的理论计算值是相近的,表明本文所给出的方法是简单的、计算结果是正确的.     

强磁场中氢原子能级的另一种绝热变分计算

采用绝热近似和变分原理，引入描述Coulomb作用的等效模型势，给出绝热变分方程，计算了均匀强磁场(1≤β≤2000)中氢原子的基态和几个较低激发态的能级，并与绝热近似方法和公认为最精确的类多组态Hartree-Fock方法的结果进行了比较，给出的基矢比Landau基矢具有更好的收敛性. 关键词：     

强磁场中氢原子的能级结构

发展了一套简单高效的非微扰理论方法研究强磁场中的原子能级结构.作为例子,给出了磁场强度从0到1000个原子单位,氢原子基态和低激发态的结合能以及四极矩等重要原子能级结构参数.结果表明:相对于其他的高精度计算方法,该方法不仅能计算出高精度的能级位置而且可方便给出精确的电子波函数.此外,该法还具有很强的普适性,可直接推广到原子与任意方向的交叉电磁场相互作用的研究. 关键词： 强磁场 CWDVR谱方法 氢原子能级结构 四极矩     

强磁场中氢原子自离化态的能级及宽度

使用Bsplines与复坐标旋转相结合的方法计算了均匀外磁场(2.35×10~6≤B≤1.175×10~4T)中氢原子│m│=0—5,偶宇称和奇宇称自离化态的能级和宽度.并与已有的结果作了比较.分析了共振态能级位置和宽度与态的宇称、磁量子数│m│及磁场强度的关系.结果表明:Bsplines与复坐标旋转方法相结合可以有效地用于强外场中原子自离化态的计算. 关键词：     

氢原子能级相对论修正的微扰方法的发散困难及其克服

指出现今所用的氢原子能级相对论效应微扰方法中蕴含着严重的发散困难，利用根式算符和动量表象克服了这种困难，重新计算氢原子各状态能级的相对论修正，并找到了前时结果在数值上所以正确的原因。     

基于高斯基展开法研究氢原子能级和波函数

本文采用高斯基展开法精确求解氢原子能级,并且研究高斯基展开法中变分参数的选取对于结果精确度的影响.程序采用Python语言编写,这一求解方法为计算物理、量子力学等课程的教学提供了参考.     

氢原子斯塔克效应中微扰矩阵元的普遍公式

讨论了任意能级下氢原子斯塔克效应中的微扰矩阵元，并给出了n=4能级的能量一级修正值。     

一维氢原子的斯塔克效应

用定态微扰理论计算了一维氢原子在均匀外电场中的斯塔克效应,并给出了一级、二级能级修正的普遍公式。     

Theoretical Calculation of Energy Levels of a Hydrogen Atom in a Strong Magnetic Field

The eleven low-lying energy levels of a hydrogen atom, and its mean radius in a uniformly high magnetic field B are calculated in a simple variational approach. The potential term containing squared magnetic field in Hamiltonian operator is separated into spherically and nonspherically symmetric potentials. The influence over levels and radius of the hydrogen atom is discussed. The results are in good agreement with the recent literatures, but more accurate. We find that the stronger the'magnetic field is, the smaller the mean radius of the hydrogen atom is.     

用B-splines技术计算超强平行外磁场中氢分子离子的能级

考虑两核之间的相互作用,采用单中心展开方法和B-splines技术构建氢分子离子的径向和角向波函数,计算超强平行外磁场中氢分子离子的能级E_b(m=0,-1,-2,-3,-4,-5)和两核间的平衡距离2R.计算中,磁场强度从2.35×10⁶T变到2.35×10⁸T.对比绝热变分近似计算结果,计算精度提高的范围在0.00015 Ry~0.0488 Ry之间;对比变分近似计算结果,计算精度提高的范围在0.0029 Ry~0.0257 Ry之间.这些计算结果表明,用二重B-splines基函数展开方法使氢分子离子的波函数的完备性更好,并能得到比绝热变分近似和绝热近似方法更高的计算精度.     

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.     

氢原子斯塔克效应的能级分裂规律

根据简并情况下的微扰理论和n=1,2,3,4能级对应的久期方程的规律,推出任意状态下氢原子斯塔克效应中的久期方程行列式中各矩阵元的分布规律,并找出了氢原子一级斯塔克效应在电场中的能级分裂规律.     

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.     

Structure of Rotating Neutron Stars in Uniform Strong Magnetic Field

Properties and deformations of the rotating neutron stars in uniform strong magnetic field are calculated. The magnetic field will soften the equation of state of the neutron star matters and make an obvious effect on the structure of the rotating neutron star. If the magnetic field is superstrong （B=10^17 T）, the mass, radius, and the deformation will become smaller effectively.     

Hydrogen atom in strong magnetic field: a high accurate calculation in spheroidal coordinates

A B-spline-type basis set method for the calculation of hydrogen atom in strong magnetic fields in the frame of spheroidal coordinates has been introduced. High accurate energy levels of hydrogen in the magnetic field, with strength ranging from 0 to 1000 a.u., have been obtained. For the ground state, 1s₀, energies with at least 11 significant digits have been obtained. For the low-lying excited state, 2p₋₁, energies with at least 9 significant digits are obtained. The method has also been applied to the calculation of hydrogen Rydberg states in laboratory magnetic fields. Energy spectra with at least 10 significant digits are presented. A comparison with other results in the literatures has been performed. Our results are comparable to the most accurate one up to date. A possible extension to the cases of parallel and crossed electric and magnetic fields have been discussed.     

Gravitational Corrections to Energy-Levels of a Hydrogen Atom

The first-order perturbations of the energy levels of a hydrogen atom in central internal gravitational field are investigated. The internal gravitational field is produced by the mass of the atomic nucleus. The energy shifts are calculated for the relativistic 1S, 2S, 2P, 3S, 3P, 3D, 4S, and 4P levels with Schwarzschild metric. The calculated results show that the gravitational corrections are sensitive to the total angular momentum quantum number.     

Calculation of Excited States of He Atoms in a Strong Magnetic Field

A recently developed B-spline algorithm is extended and utilized to calculate excited states of He atoms in the presence of strong magnetic fields. Binding energies are presented for He in the five excited atomic states 2¹0⁺, 1¹0^-, 2¹0^-, 1¹(-1)⁺, and 2¹(-1)⁺ with magnetic field strength ranging from 0.0001 to 10 a.u. The obtained energies are compared with available theoretical data, and found to be in good agreement. We investigate influence of magnetic fields on atomic structures of multielectron atoms, and illustrate that how electron probability density distributions change with increasing magnetic field strength. The current approach is directly applicable to simulations of discrete spectra for He atoms in the atmospheres of magnetized white dwarf stars.