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The theory of line shapes relevant to the spectra of cool stars

机译：与冷星光谱有关的线形理论

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Accurate pressure broadened profiles of alkali resonance doublets are needed for modelling of the atmospheres of cool stars and for generating their synthetic spectra in the region 400-900 nm. When the usual impact theory of line broadening is used, the profile is simply Lorentzian and the widths and shifts of the lines can be calculated, provided that interaction potentials for the emitter-perturber system are available. However when the lines utterly dominate their region of the spectrum, it becomes important to also accurately represent the profile in the line wings, where the impact theory is no longer valid. The original development of line broadening theory by Baranger in 1958 is reexamined and calculations have been carried out in which it is shown that it is not necessary to invoke the impact approximation. To test the validity of different approximations, results for line widths and shifts are presented for the lithium and sodium resonance lines broadened by helium for 0.1 K ≤T≤ 3000 K.
机译：为了模拟冷星大气并生成其在400-900 nm范围内的合成光谱，需要碱共振双峰的准确的压力展宽曲线。当使用常规的线展宽影响理论时，轮廓可以简单地称为洛伦兹曲线，并且可以计算出线的宽度和位移，前提是可以使用发射极-扰动系统的相互作用势。但是，当线条完全支配它们的光谱区域时，重要的是也必须准确地表示线条翼中的轮廓，在该处冲击理论不再有效。重新研究了Baranger在1958年提出的线展宽理论，并进行了计算，结果表明没有必要援引影响近似。为了测试不同近似值的有效性，给出了在0.1 K≤T≤3000 K的条件下，氦原子加宽的锂和钠共振线的线宽和位移的结果。

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