Calcul des intensités des transitions laser dans 12C16O2 et ses molécules isotopiques

1984 ◽  
Vol 62 (4) ◽  
pp. 736-740 ◽  
Author(s):  
Philippe Millie
Keyword(s):  
Emission Line ◽  
Potential Function ◽  
Laser Emission ◽  
Transformation Method ◽  
Wave Functions ◽  
Contact Transformation ◽  
Line Intensities ◽  
Laser Emission Line

The laser emission-line intensities of 12C16O2 and several isotopes were theoretically calculated. The vibrational wave functions were obtained to a direct diagonalization by utilizing a previously known potential function. These values are compared to the experimental ones. The effect of electrical anharmonicity is discussed. The validity of the contact transformation method is briefly analyzed.

scholarly journals IUE Spectra of The by Dra/Flare Star AU Mic

1983 ◽  
Vol 71 ◽  
pp. 249-250
Author(s):  
C.J. Butler ◽  
A.D. Andrews ◽  
J.G. Doyle ◽  
P.B. Byrne ◽  
J.L. Linsky ◽  
...  
Keyword(s):  
Light Curve ◽  
Emission Line ◽  
Flare Star ◽  
Emission Lines ◽  
Spectral Variation ◽  
Strong Emission ◽  
Line Intensities ◽  
The Mean ◽  
Phase Interval

A coordinated series of ground-based optical and IUE observations of BY Dra variables was undertaken to follow the spectral variation of these stars over one cycle. In the first series 20 LWR and 19 SWP trailed spectra were taken of AU Mic over a three day period 4-6 August 1980 .In Figure 1 we show the mean integrated fluxes for the strong emission lines in the SWP spectra of AU Mic over the observed phase interval of 0.14 to 0.8 together with an approximate V light curve determined by the FES on IUE. From comparison of the emission line intensities and FES magnitudes in Figure 1 several points emerge.

Theoretical Helium i Emission-Line Intensities for Quiescent Prominences

1974 ◽  
Vol 192 ◽  
pp. 181 ◽  
Author(s):  
J. N. Heasley ◽  
Dimitri Mihalas ◽  
A. I. Poland
Keyword(s):  
Emission Line ◽  
Line Intensities

Transition probabilities for lines arising from the 3d4 4p configuration of Cr(II)

1994 ◽  
Vol 72 (1-2) ◽  
pp. 57-60 ◽  
Author(s):  
A. M. Gonzalez ◽  
M. Ortiz ◽  
J. Campos
Keyword(s):  
Experimental Data ◽  
Emission Line ◽  
Sum Rules ◽  
Transition Probabilities ◽  
Line Strength ◽  
Line Intensities ◽  
Cr Content ◽  
Absolute Scale ◽  
Relative Transition ◽  
Thin Plasma

Relative transition probabilities for 43 lines arising from the 3d4 4p configuration of Cr(II) with cores 3d4 (5D), 3d4 (3P), and 3d4 (3H) were determined from measurements of emission-line intensities in a laser produced plasma. This experiment was carried out with Al–Cr alloys with a Cr content of about 0.1%, in order to have an optically thin plasma. Transition probabilities were placed on an absolute scale by using, where possible, accurate experimental lifetimes from the literature and line-strength sum rules. Comparison of the present results with the available theoretical and experimental data are made.

scholarly journals UV and optical spectrum variability of T Tau and RY Tau

2012 ◽  
Vol 8 (S292) ◽  
pp. 44-44
Author(s):  
N. Z. Ismailov ◽  
N. Kh. Quliyev ◽  
O. V. Khalilov ◽  
H. N. Adigezalzade
Keyword(s):  
Emission Line ◽  
Brightness Variation ◽  
Emission Lines ◽  
Spectral Energy ◽  
Spectral Radiation ◽  
Line Intensities ◽  
T Tauri ◽  
Spectral Ranges ◽  
T Tau ◽  
Archive Data

AbstractIn this report we have presented results of spectral observations of classical T Tauri type stars T Tau and RY Tau. Observational dates were obtained from following sources: spectrograms of the UV range from the IUE archive data, and spectrograms of the visual range obtained in the 2 m telescope of ShAO of the NAS of Azerbaijan (Ismailov et al. 2010). For both of stars on the Scargle method we have searched a periodicity of variations in equivalent widths of emission lines in the optical and UV ranges. In the RY Tau firstly was detected the periodic variability in MgII λ2800 Å emission doublet intensities with a period of 23 days. The observed period had also revealed with the equivalent widths and displacements of components of Hα and H+Hϵ and K CaII emission.The lines were found to be shifted to short wavelengths as the emission line intensities increased in both UV and optical spectral ranges. The lack of a correlation between the brightness variation and the emission line intensity also suggests that, on the whole, the contribution from the radiation in emission lines for the star RY Tau is insignificant.On the analysis of T Tau we conclude that there is a significant variation of spectral emission lines in the optical and UV on a time scale of about 33 days and that this variations is periodic. Both of stars shows the periodicity also for observed group of such lines as CIV λ1450 Å, HeII λ 1640 Å, SII λ1756 Å (Ismailov et al. 2010, Ismailov et al. 2011).Additionally we have carried out spectral energy distributions of this stars in the range 0.36-100 μm which have indicated the excess of spectral radiation in the IR range of spectrum. These excesses of radiations can be explained by the thermal radiation of still unformed bodies at the circumstellar environment. The periodic variability in the spectrum together with the excess of the spectral radiation may be occurred by protoplanets and/or protostars in these young systems. It is showed that possible, planet formation processes mainly to be completed at the time of the formation of classical T Tauri type stars.

Atomic Data and Emission‐Line Intensities for Cavii

2003 ◽  
Vol 589 (2) ◽  
pp. 1075-1084 ◽  
Author(s):  
E. Landi ◽  
A. K. Bhatia
Keyword(s):  
Emission Line ◽  
Atomic Data ◽  
Line Intensities

Anharmonic potential constants and the large amplitude bending vibration in nitrogen dioxide

1976 ◽  
Vol 54 (1) ◽  
pp. 80-91 ◽  
Author(s):  
J. L. Hardwick ◽  
J. C. D. Brand
Keyword(s):  
Nitrogen Dioxide ◽  
Potential Function ◽  
Large Amplitude ◽  
Perturbation Expansion ◽  
Hamiltonian Operator ◽  
Wave Functions ◽  
Bending Vibration ◽  
Equilibrium Bond Length ◽  
Anharmonic Potential ◽  
Set Up

The anharmonic potential function of the ground electronic state of nitrogen dioxide has been determined within the framework of three different vibrational Hamiltonians. The first of these, which involves a perturbation expansion of the vibrational wave functions in terms of normal coordinate harmonic oscillator wave functions, is the most widely used and generally applicable of the three. It suffers, however, from demonstrably large systematic errors. The other two are vibration–rotation Hamiltonians which allow explicitly for a large amplitude vibration in the bending vibration of a triatomic molecule; they set up the Hamiltonian operator as an explicit function of the bond angle and solve the Schrödinger equation numerically. The more sophisticated of these, the so-called nonrigid bender Hamiltonian, reproduces the spin-free virtual term values to the (0, ν2, 0) manifold of 14NO2 to a standard deviation of 0.026 cm−1 for states with N ≤ 10 and ν2 ≤ 3. It is, moreover, observed to be a more useful tool for extrapolation than is the ordinary parametrized Hamiltonian.The potential function for the bending coordinate is defined by αe = 133.888 ± 0.002°, fαα = 1.61022 ± 0.00005 mdyn Å/rad2, fααα = −2.1172 ± 0.0003 mdyn Å/rad3, and fαααα = 6.0228 ± 0.0020 mdyn Å/rad4. The equilibrium bond length, re, is found to be 1.19464 ± 0.00015 Å.

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