Influence of a small inhomogeneous broadening of Cr 3+ :LiSrAlF 6 emission line on the laser performance
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Homogeneous broadening
The broadening mechanism of a prominence Hα line is mainly a combination of Doppler broadening and damping broadening, and Stark broadening can be neglected. In this paper, the relationships between an Hα self-reversal line of a solar prominence and its broadening mechanism are discussed. It is found that the characteristics of the prominence self-reversal line are not affected by any of the broadening mechanisms used, and, in general, the profile shape of the prominence Hα line with deep self-reversal is hardly changed by any of the broadening mechanisms used. The calculated parameters, such as the distance between the two peak points of a self-reversal line and the Doppler width of the line, are changed even less, i.e. the effects of broadening mechanisms on the prominence self-reversal line are very small. For the prominence line with shallow self-reversal, however, the profile shape is changed with any of the different broadening mechanisms used, i.e. the shallow hump is obviously changed, and the calculated parameters are greatly changed.
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Stark broadening parameters have been calculated for 60 spectral lines of Xe viii, for broadening by electron, proton, and He iii impacts. For calculations, the semiclassical perturbation approach in the impact approximation has been used. The widths and shifts are provided for temperatures from 20 000 K to 500 000 K and for an electron density of 1017 cm−3. Obtained results have been used to study the influence of Stark broadening on spectral lines in DO white dwarf atmospheres and it has been found that exist broad layers where this broadening mechanism is dominant in comparison with thermal Doppler broadening.
Homogeneous broadening
Semiclassical physics
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The broadening mechanism of a prominence Ha line is mainly a combination of Doppler broadening and damping broadening, and Stark broadening can be neglected. In this paper, the relationships between an H alpha self-reversal line of a solar prominence and its broadening mechanism are discussed. It is found that the characteristics of the prominence self-reversal line are not affected by any of the broadening mechanisms used, and, in general, the profile shape of the prominence H alpha line with deep self-reversal is hardly changed by any of the broadening mechanisms used. The calculated parameters, such as the distance between the two peak points of a self-reversal line and the Doppler width of the line, are changed even less, i.e. the effects of broadening mechanisms on the prominence self-reversal line are very small. For the prominence line with shallow self-reversal, however, the profile shape is changed with any of the different broadening mechanisms used, i.e, the shallow hump is obviously changed, and the calculated parameters are greatly changed.
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Line (geometry)
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In this paper the Doppler and Stark broadening mechanisms of HeI 10830Angstrom are discussed and various broadening parameters calculated. The following conclusions are drawn: compared to the Doppler effect, the action of radiative damping on the broadening of HeI 10830Angstrom can be neglected. For the generally acknowledged value of electron density of flares (N-e = 3.2 x 10(13) cm(-3)), none of the damping terms can produce any discernible broadening. Up to N-e = 10(15) cm(-3), none of the various types of damping can effect an increase in the half-width of the line center, and the maximum increase is of the order of 10(-3)Angstrom. Therefore, the broadening at the line center may always be thought to be Doppler broadening. When N-e > 10(14) cm(-3), Stark broadening, especially the Stark broadening of electrons, plays the chief role in the broadening of HeI 10830Angstrom. If the wings of the Stark-broadened profile are to be 2-3 times larger than those of the purely Doppler-broadened profile, then the half-width of damping broadening should be comparable to Deltalambda(D). If the observed profile of the limb flare of 1989 is interpreted as Stark broadening, then the electron density would be as high as 10(17) cm(-3). The collisional damping (gamma(3)) with helium atoms causes clearly different amounts of broadening on the components I-12 and I-3: the effect is one order of magnitude higher on I-12 than on I-3. But our observation shows that the wing extensions of I-12 and I-3 are basically the same, so it is impossible that our observed profile is produced by gamma(3).
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The Doppler broadening, Stark broadening and various kinds of broadening parameters of HeI 10830 A line in solar flare are calculated and discussed and consequently the following results are got: radiation damping can be neglected when compared with Doppler broadening, and in the case of generally accepted electron density in a solar flare (Ne= 3.2 ×1013 cm3 ), all the damping terms will not lead to distinguishable broadening in the HeI 10830 A profile. All the damping effects will not result in discernible increment of the half width of HeI 10830 A until the electron density reaches to 1015 cm3 when the largest increment is about 10-3A. Therefore. the line center of HeI 10830 A line can be taken as Doppler broadening. When electron density is greater than 1014 cm3 , Stark broadening, especially that by electron collisicn, will play a major role in the broadening of HeI 10830 A line. In order for the half width of the line resulted from Stark broadening to be 1-2 times greater than that from Doppler broadening, the half width from damping effect will be equivalent to that from Doppler effect. Consequently, the electron density will be of the order of 1017 cm3 if we interpret the observed HeI 10830 A profiles in the 1989 limb flare by Stark broadening. Broadening effect caused by collision with helium atom (γ3) has different impact on I12 and I3 component. The impact on I12 is about one order greater than that on 13. The observed HeI 10830 A profiles of 1989 limb flare show that I12 and I3 have almost the same extended profile, therefore, they can not result from γ3.
Homogeneous broadening
Line (geometry)
Solar flare
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Homogeneous broadening
Spectral hole burning
Asymptote
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The Doppler broadening, the natural broadening, and the quasi-static broadening are introduced. The last broadening is due to the Stark effect in the Holtsmark micro-field with the Debye shielding. Plasma electrons give rise to the impact broadening, which is discussed in detail. For neutral hydrogen and hydrogen-like ions for which the linear Stark effect is dominant, the quasi-static broadening tends to be important. For other atom (ion) species, which are subjected to the quadratic Stark effect, the impact broadening tends to be dominant. The Inglis-Teller limit, which results from the line broadening becoming comparable with the line separation, is useful for a rough estimate of plasma density. Convolution of a Lorentzian profile and a Gaussian profile yields a Voigt profile.
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Debye
Voigt profile
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Homogeneous broadening
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Solar flare
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We investigate broadening phenomena of spectral holes burned into delocalized states of molecular aggregates. We measured spectral-diffusion broadening, homogeneous line broadening, and pressure-induced line broadening. The behavior is quite different from that for localized states. Whereas homogeneous broadening is dominated by exciton–phonon scattering, spectral-diffusion broadening and pressure broadening are extremely small because of large motional narrowing effects.
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Line (geometry)
Motional narrowing
Spectral line shape
Spectral hole burning
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Several reasons for atomic spectral line broadening in terms of theory are given, that's: natural broadening: Doppler broadening; collision broadening, respectively. Some estimated data based on these reasons are provided, which may be of significance for atomic spectral measurements, and the data are in agreement with experiments.
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