The Paschen–Back effect in helium spectra revisited

2002 ◽  
Vol 80 (11) ◽  
pp. 1383-1389 ◽  
Author(s):  
V D Ovsiannikov ◽  
E V Tchaplyguine
Keyword(s):  
Hilbert Space ◽  
Fine Structure ◽  
Field Strength ◽  
Quantum Number ◽  
Complete Information ◽  
Numerical Calculations ◽  
Magnetic Quantum Number ◽  
Helium Spectra ◽  
Line Positions

The complete information for the intensities of the Zeeman components in the helium triplet lines corresponding to the radiation transitions n3 PJM [Formula: see text] n' 3S1M ' is analyzed in the field-strength region from anomalous Zeeman effects to complete Paschen–Back effects. The diagonalization of the paramagnetic interaction for n3PJM was carried out for the states with magnetic quantum number M = 0 in the Hilbert space of dimension 3, taking account of all three fine-structure sublevels, J = 0,1,2. The results of the numerical calculations for line positions and intensities are presented in a table and figures. The departure from the previously known data is discussed. PACS Nos.: 32.60+i, 32.70Fw, 32.30-r

A Discussion on solar studies with special reference to space observations - The manifold structure of the chromosphere and corona

1971 ◽  
Vol 270 (1202) ◽  
pp. 77-80 ◽  
Keyword(s):  
Magnetic Field ◽  
Fine Structure ◽  
High Resolution ◽  
Field Strength ◽  
Special Reference ◽  
Velocity Fields ◽  
Field Patterns ◽  
Uniform Region ◽  
Determining Factor ◽  
The Magnetic Field

Although the photosphere is a uniform region for scales greater than the granulation, the fact that the magnetic field strength falls off less sharply than the gas pressure leads to strong magnetic influence at greater heights in the solar atmosphere. This magnetic influence leads to non-uniformity and fine structure in the chromosphere and corona. The existence of such structure has been deduced mostly from measurements of photospheric phenomena; in particular, from measurements of photospheric velocity fields (Leighton, Noyes & Simon 1962) and of photospheric magnetic fields (Bumba & Howard 1965). The determining factor would thus appear to be in the photosphere; but visible effects only are produced in the chromosphere and corona. In recent years, high resolution filter photography has enabled us to recognize different regions of the chromosphere, where qualitatively different structure is associated with distinct magnetic field patterns. This progress has been possible because of better Lyot filters, better films and better observing sites; the spectroheliograph has always been limited for high resolution work by the finite slit width and the difficulty of accurate guiding during the long exposures.

Ligand-Field Strength and Symmetry-Restricted Covalency in CuIIComplexes - a Near-Edge X-ray Absorption Fine Structure Spectroscopy and Time-Dependent DFT Study

2015 ◽  
Vol 2015 (16) ◽  
pp. 2707-2713 ◽  
Author(s):  
Giulia Mangione ◽  
Luciano Pandolfo ◽  
Mauro Sambi ◽  
Giovanni Ligorio ◽  
Marco Vittorio Nardi ◽  
...  
Keyword(s):  
Fine Structure ◽  
Field Strength ◽  
Time Dependent ◽  
Dft Study ◽  
Ligand Field ◽  
X Ray ◽  
Absorption Fine ◽  
X Ray Absorption

Analytical formulas for the Stark effect on intensity of hydrogen radiation lines

2003 ◽  
Vol 81 (5) ◽  
pp. 755-769 ◽  
Author(s):  
A A Kamenski ◽  
V D Ovsiannikov
Keyword(s):  
Perturbation Theory ◽  
Green Function ◽  
Field Strength ◽  
Stark Effect ◽  
Selection Rule ◽  
Magnetic Quantum Number ◽  
Matrix Elements ◽  
Analytical Formulas ◽  
Degenerate States ◽  
Analytical Expressions

A regular method for deriving the consecutive terms of a series in powers of field strength F for the intensities of hydrogen radiation lines is presented both analytically and numerically. Specific modification of the perturbation theory for degenerate states and the Sturm-series expansion for the completely reduced Coulomb–Green function in parabolic coordinates are used to derive simple analytical formulas for matrix elements and the intensities of the radiation transitions between circular states. Particular cases of transitions between the closest Rydberg levels are presented and discussed in detail. Analytical expressions are also derived for the quadrupole matrix elements, which may contribute to the probability of σ-transitions with the selection rule for the magnetic quantum number Δm = ±1 and determine the probability of the dipole-forbidden radiation transitions between Stark levels with Δm = ±2. PACS Nos.: 32.60.+i, 32.70.–n, 32.70.Fw

scholarly journals Колебательно-вращательный спектр высокого разрешения в районе полос 3ν-=SUB=-4-=/SUB=-, ν-=SUB=-2-=/SUB=-+2ν-=SUB=-4-=/SUB=- и 2ν-=SUB=-2-=/SUB=-+ν-=SUB=-4-=/SUB=- молекулы -=SUP=-72-=/SUP=-GeH-=SUB=-4-=/SUB=-

2022 ◽  
Vol 130 (3) ◽  
pp. 345
Author(s):  
А.В. Кузнецов ◽  
Н.И. Распопова ◽  
О.В. Громова ◽  
Е.С. Бехтерева ◽  
М.А. Кошелев ◽  
...  
Keyword(s):  
High Resolution ◽  
Quantum Number ◽  
Optical Resolution ◽  
Rotational Structure ◽  
High Resolution Spectrum ◽  
Effective Hamiltonian ◽  
Rotational Bands ◽  
Fitting Procedure ◽  
Maximum Value ◽  
Line Positions

The high-resolution spectrum of the 72GeH4 molecule was recorded on a Bruker IFS 125HR Fourier spectrometer with an optical resolution of 0.003 cm-1. The line positions were analyzed for ten interacting vibrational-rotational bands 3ν4 (1F2, F1, 2F2), v2+ 2ν4 (1E, F1, F2, 2E) and 2ν2+v4 (1F2, F1, 2F2) in the range 2350-2750 cm-1. As a result of the analysis, 1726 experimental lines were identified with the maximum value of the quantum number Jmax = 17; then used in the fitting procedure with parameters of the effective Hamiltonian. The resulting set of 35 spectroscopic parameters describes the vibrational-rotational structure of the spectrum with drms = 7.5 · 10-4 cm-1.

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