Reinvestigation of pressure broadening parameters at 60-GHz band and single 118.75 GHz oxygen lines at room temperature

Low pressure measurements of broadening parameters of the 118.75 GHz fine structure line of oxygen molecule have been made by a BWO-based spectrometer with acoustic detector (RAD) at room temperature. Pressure broadening parameters were obtained for the buffer gases O₂, N₂, Ne, He, Ar, H₂O, CO₂, and CO and have the following values 2.23 ± 0.01, 2.245 ± 0.02, 1.375 ± 0.02, 1.62 ± 0.03, 2.005 ± 0.02, 2.52 ± 0.04, 2.66 ± 0.08, and 2.31 ± 0.05 MHz/Torr, respectively. Measured central frequency is 118 750.340 ± 0.007 MHz. The central frequencies and broadenings by O₂ and N₂ of fine structure lines 1⁺, 5⁻, 7⁺, 11⁺, and 15⁻ belonging to the 60-GHz band are also measured. Comparison of previous and recent data on electronic, rotational, and fine structure lines broadenings reveals their close values (within 10%) and dependencies on corresponding rotational quantum numbers for these different oxygen spectra stretching from millimeter through submillimeter up to the optical bands. Such similarity could be used for estimation of the broadenings of not measured yet oxygen lines.     

Spectroscopically determined potential energy surfaces of the H2O, H2O, and H2O isotopologues of water

Adiabatic potential energy surfaces (PESs) for three major isotopologues of water, H₂¹⁶O, H₂¹⁷O, and H₂¹⁸O, are constructed by fitting to observed vibration-rotation energy levels of the system using the nuclear motion program DVR3D employing an exact kinetic energy operator. Extensive tests show that the mass-dependent ab initio surfaces due to Polyansky et al. [O.L. Polyansky, A.G. Császár, S.V. Shirin, N.F. Zobov, P. Barletta, J. Tennyson, D.W. Schwenke, P.J. Knowles, Science 299 (2003) 539-542.] provide an excellent starting point for the fits. The refinements are performed using a mass-independent morphing function, which smoothly distorts the original adiabatic ab initio PESs. The best overall fit is based on 1788 experimental energy levels with the rotational quantum number J = 0, 2, and 5. It reproduces these levels with a standard deviation of 0.079 cm⁻¹ and gives, when explicit allowance is made for nonadiabatic rotational effects, excellent predictions for levels up to J = 40. Theoretical linelists for all three isotopologues of water involved in the PES construction were calculated up to 26 000 cm⁻¹ with energy levels up to J = 10. These linelists should make an excellent starting point for spectroscopic modelling and analysis.     

The ν5 and 2ν9 bands of the N isotopic species of nitric acid (H15NO3): Line positions and intensities

Nitric acid (HNO₃) plays an important role in the Earth’s atmosphere as a reservoir molecule of NO_x species. It has a strong infrared signature at 11 μm which is one of the most commonly used for the infrared retrieval of this species in the atmosphere since this spectral region coincides with an atmospheric window. It is therefore essential to have high quality spectral parameters in this spectral region. For the H¹⁴NO₃ (main) isotopic species, the 11 μm bands were already the subject of numerous extensive studies which involve not only the ν₅ and 2ν₉ cold bands but also the first hot bands. The present work is the first high resolution Fourier transform analysis of the 11 μm bands for H¹⁵NO₃, which is the second most abundant isotopomer of nitric acid [a ≅ 0.00365(7)]. In this way, the analysis of the ν₅ and 2ν₉ cold bands centered at 871.0955 and 893.4518 cm⁻¹ was performed, and as for H¹⁴NO₃, these bands are significantly perturbed since rather strong resonances couple the 5¹ and 9² rotational levels. The theoretical model that we used to compute the line positions and line intensities is directly issued from the one which we used recently for H¹⁴NO₃ [A. Perrin, J. Orphal, J.-M. Flaud, S. Klee, G. Mellau, H. Mäder, D. Walbrodt, M. Winnewisser, J. Mol. Spectrosc. 228 (2004) 375-391]. Actually, for the H¹⁵NO₃ line positions, the Hamiltonian matrix accounts for the rather strong Fermi and the weaker Coriolis interactions linking the 5¹⇔9² rotational levels. Using this model which accounts correctly for the strong mixing of the 5¹ and 9² upper state energy levels, the ν₅ and 2ν₉ line intensities for H¹⁵NO₃ were satisfactorily computed using the ν₅ and 2ν₉ transition moment operators achieved previously for the ¹⁴N (main) isotopic species. In this way, the transfer of intensities from the ν₅ fundamental (and presumably strong) band to the 2ν₉ overtone (and presumably weak) band could be explained for H¹⁵NO₃ as it was done previously for the ¹⁴N (main) isotopic species. Finally, the position of the H¹⁵NO₃ν₅ + ν₉ − ν₉ hot band was identified at 875.245 cm⁻¹.     

CO2 line intensity FTS measurements with 1% assumed accuracy in the 1.5-1.6 μm spectral range

Using Fourier-transform spectra and a multispectrum fitting procedure, 124 absolute line intensities of ¹²C¹⁶O₂ are obtained for the cold band 30011-00001 and the hot band 01131-01101 between 6460 and 6950 cm⁻¹. Vibrational transition dipole moments squared and Herman-Wallis coefficients are reported for each band. Cross comparisons made with previous experimental results and with data available in the HITRAN and Carbon Dioxide Spectroscopic Databank (CDSD), bring some confidence on the good level of accuracy of the present results. Motivated by the demanding needs of some atmospheric experiments dedicated to the survey of the carbon cycle, an additional evaluation of potential absolute line intensity measurement limit is also performed on recently published carbon dioxide absolute line intensity independent measurements. These are obtained in two different laboratories on the bands 30013-00001 and 30012-00001 both located in the 1.6 μm spectral window. It is shown that Fourier-transform experimental CO₂ line intensity determination is approaching the challenging required figure of about 0.3% accuracy needed for the survey of the atmospheric carbon cycle.     

马氏定律与哈勃定律的辨析

本文从理论,实验上论证了“马氏（红移）定律”,同时指出所谓“退行速度Vr”或“星系红移”与“星系间的距离”无必须的关系,从这个意义上来说,哈勃定律是错误的。     

顺序等离子体光谱技术测定煤飞灰中常量,少量和微量元素

本文采用顺序等离子体光谱技术测定煤飞灰中主要成份（Ｃａ、Ｍｇ、Ｆｅ、Ａｌ、Ｓｉ、Ｎａ、Ｋ、Ｔｉ）及微量成份（Ｃｕ、Ｓｃ、Ｖ、Ｎｉ、Ｂｅ、Ｍｎ）。用扫描光谱法研究了分析线的选择和光谱背景的扣除。试样用密封罐混酸溶解。测定煤飞灰标准样品ＮＢＳ１６３３ａ的结果与标准值一致。方法用于测定新制备的煤飞灰标准参考物。     

利用谱线宽度测人发中的微量元素

通过实验证明了可以利用谱线宽度做永久工作曲线用于光谱定量分析。给出了用于测量人发中微量元素Ｃｕ，Ｚｎ，Ｆｅ和Ｃａ的永久工作曲线，利用这些工作曲线对实际样品进行了测定，所得结果与用ＩＣＰ－ＡＥＳ测得的结果相吻合。     

上层大气中铁质流星尾迹的紫外光谱模拟

基于 Sparrow理论 ,计算了海拔 90— 95 km高空的不同初始地心坐标速度的典型铁质流星的有效温度 ,获得初速 72 km/ s的该类流星尾迹主要成分的粒子数密度 ,以 Cloudy程序模拟了该流星尾迹的 2 0 0—4 0 0 nm波段紫外辐射 ,给出了若干预期的强谱线的相对强度     

关于带有完全对称函数的广义数值域

本文给出了矩阵Ａ的带有完全对称函数Ｃｋ的ｍ－数值域在复平面上为线段的充分必要条件．     

光谱法研究氢等离子体循环机制

利用多道光学分析仪测量Hα线形分布,从线形的分布推出再循环的氢原子主要来源于离子中性化后的反射和氢分子的离解。通过双高斯拟合H_α线形分布,由多普勒频移得出了氢原子的入射速度。从氢原子能量分布上的特征峰得出氢分子的离解方式主要是电离和直接离解。