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Physical Review A

Pressure dependence of Na resonance line broadening by Kr and Xe

W.P. West, Alan C. Gallagher

Published Apr 1, 1978• 35 citations
Publisher

Abstract

The fluorescent spectrum of the Na $D$ lines, pressure broadened by Xe and Kr, has been measured for noble-gas densities of 2\ifmmode\times\else\texttimes\fi{}${10}^{19}$-3\ifmmode\times\else\texttimes\fi{}${10}^{20}$ ${\mathrm{cm}}^{\ensuremath{-}3}$; at the lower density, the lines are isolated while, at the higher, they are severely blended. The spectra are obtained in normalized intensity units allowing the nonbinary behavior of the line wing intensity to be clearly observed. At the lower density the broadening is well characterized by isolated binary interactions; at the higher density multiple-perturber interactions dominate. Nonlinearities in the pressure dependence of shifts, widths, and satellite shape are reported.

DOI
10.1103/physreva.17.1431

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The fluorescent spectrum of the Na DDD lines, pressure broadened by Xe and Kr, has been measured for noble-gas densities of 2\ifmmode\times\else\texttimes\fi{}1019{10}^{19}1019-3\ifmmode\times\else\texttimes\fi{}1020{10}^{20}1020 cm\ensuremath−3{\mathrm{cm}}^{\ensuremath{-}3}cm\ensuremath−3; at the lower density, the lines are isolated while, at the higher, they are severely blended. The spectra are obtained in normalized intensity units allowing the nonbinary behavior of the line wing intensity to be clearly observed. At the lower density the broadening is well characterized by isolated binary interactions; at the higher density multiple-perturber interactions dominate. Nonlinearities in the pressure dependence of shifts, widths, and satellite shape are reported.
The normalized fluorescence spectrum of the Li 6708-\AA{} resonance line perturbed by the noble gases has been measured for 100 \AA{} either side of the resonance line, at a temperature of 400 \ifmmode\pm\else\textpm\fi{} 10\ifmmode^\circ\else\textdegree\fi{}C. The noble-gas pressure range of 100-1800 Torr was investigated. It was observed that the line wings scale linearly with this pressure for $2<|\ensuremath{\Delta}\ensuremath{\lambda}|<100$ \AA{}, and it was was demonstrated that a Lorentzianbroadened line core can be observed for this pressure range. The Li density was \ensuremath{\sim} 1010{10}^{10}1010/cm3{\mathrm{cm}}^{3}cm3 and was varied to establish the fluorescence spectrum in the limit of no radiation entrapment. The central region of the line has been measured with high resolution and compared to calculated profiles due to the various fine structure and isotopic line components, each broadened by a convolution of Lorentz, Doppler, and instrumental profiles. The shift and Lorentz broadening rates, as well as the wavelengths for transition to non-Lorentzian behavior, are reported. In contrast to the heavier alkali-metal-noble-gas cases, no distinctive far-wing features such as satellites or sharp inflections are observed. This is consistent with the much larger collision velocities for the Li case.
Normalized emission spectra of the optically excited Rb resonance lines (7800 \AA{}, 7948 \AA{}) have been measured in the presence of He, Ne, Ar, Kr, and Xe for about 50 \AA{} on either side of the lines. The perturber gas pressures were in the range 100-1100 Torr and the temperature was 318 \ifmmode^\circ\else\textdegree\fi{}K. The spectra, normalized to the total emission, are shown to be due to binary collisions. Shifts and widths of the Lorentzian cores of the lines were obtained, at pressures sufficiently low for impact theory to apply. The widths are corrected for the Rb hfs and the instrument function. Various power-law fits to the near-wing intensities are presented and compared to theoretical expectations. The red satellites reported by other authors are found to be, in the low-pressure limit, mere shoulders on the line wing for Ar and Kr, while Xe barely produces an actual peak. The measured linewidths and shifts are compared to previous measurements.
We studied the line shape of Rb D1{D}_{1}D1​ and D2{D}_{2}D2​ resonance lines in the presence of 1--10 amg of several gases: 3{}^{3}3He, 4{}^{4}4He, N2{}_{2}2​, and Xe. We found that the line cores are well described by the asymmetric line shape expected for a van der Waals interatomic potential. The width and shift of the lines is proportional to the density of the foreign gas with high degree of accuracy, while the asymmetry is independent of the density. The constants of proportionality for pressure broadening and shift were measured with much higher accuracy than in previous experiments. We also studied the density dependence of the oscillator strength of the transitions.
The fluorescent spectra of the Cs principal series lines 4555 and 4593 AA (72P32,1/2/-62S12/) broadened by Kr and Xe were measured up to perturber gas densities of about 4.9*1019 cm-3. In addition, the absorption spectra of the Cs principal series line 3876 AA (62S12/-82P32/) broadened by Xe (1.63*1018<or=NX3<or=1.9*1019 cm-3) were investigated. The existence of secondary satellites was established. The intensity dependence of the quasistatic wings is discussed and qualitatively explained by competitive additive two- and three-body interactions.
The shapes of the thallium (Tl) 535- and 377.6-nm resonance lines broadened by 500-1500 Torr of noble gases have been measured at 743 K. The reported normalized emission intensities yield absorption coefficients in absolute units for all portions of the line. The shift and broadening of the Lorentzian-shaped line cores, the wavelengths of the transition to non-Lorentzian wings, wing shapes, and satellite positions, shapes, and intensities are reported. As an example, a pair of excited and ground-state interaction potentials are given for the Xe case to explain the shift, width, and intensities in all portions of the line wings.
Measurements are presented for the blue-wing satellite bands of the Rb first resonance line (780 nm) emitted in the presence of the noble gases Ne, Ar, Kr, and Xe. The continuum intensity per spectral interval and perturber density is expressed as a fraction of the total Rb (780 nm) fluorescence from optically thin vapor. Over the \ensuremath{\sim}1018{10}^{18}1018-1019{10}^{19}1019 cm3{\mathrm{cm}}^{3}cm3 density range investigated this normalized satellite-peak intensity is found to scale linearly with perturber density and approximately exponentially in $\frac{\ensuremath{-}1}{T},T$ being the absolute temperature. In the classically forbidden region beyond the satellite peak the intensity drops exponentially with frequency for Xe perturbers, but departs from exponential behavior in the Ar and Kr data. We observe undulations in the spectra between line center and the satellite. This is expected due to the possibility of interference between contributions to the transition probability at two internuclear separations, the separations at which the difference potential equals the photon energy.