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Isotopomer lowest

H3 (and its isotopomers) and the alkali metal triiners (denoted generally for the homonuclears by X3, where X is an atom) are typical Jahn-Teller systems where the two lowest adiabatic potential energy surfaces conically intersect. Since such manifolds of electronic states have recently been discussed [60] in some detail, we review in this section only the diabatic representation of such surfaces and their major topographical details. The relevant 2x2 diabatic potential matrix W assumes the fomi... [Pg.584]

In this section, we extend the above discussion to the isotopomers of X3 systems, where X stands for an alkali metal atom. For the lowest two electronic states, the permutational properties of the electronic wave functions are similar to those of Lij. Their potential energy surfaces show that the baniers for pseudorotation are very low [80], and we must regard the concerned particles as identical. The Na atom has a nuclear spin " K, and K have nuclear... [Pg.604]

The 27-cliads in the vibrational Raman spectrum of CO2 and its isotopic variants were measured and their intensity distribution simulated (Srinivasan et al., 1977 Finsterholzl et al., 1978 Kldckneret al., 1978 Finsterholzl, 1982 Wienecke et al., 1986). In Fig. 4.3-25 the experimental and the calculated Raman spectra of natural CO2 in the Fermi resonance region are presented, the lowest (calculated) spectrum showing only the 2-branches of the Fermi doublet of C 02 and its hot bands and those of the isotopomers C 02, and occuming in natural abundances of 1.1 %, 0.4 %, and 0.08 %,... [Pg.288]

Detailed resonance Raman spectra of these complexes, including those of the 0 and CDj isotopomers of the triphenylphosphine complex, have been recorded and assignments for the key skeletal modes have been made [52, 77]. We will determine the geometric changes attendant upon excitation into the lowest allowed electronic transition (approx. 370 nm), the transition being known to be axially polarized [52] and thus considered to be the lowest A2u transition with largely d 2 - dj2(<7 (Rh2) - o(Rh2)) parentage... [Pg.177]

Loren, Mundy and Plambeck [110] to estabhsh the presence of the ion in interstellar clouds. The lowest rotational transitions in the isotopomers C 0+ and were studied subsequently by Piltch, Szanto, Anderson, Gudeman, Dixon and Woods [111]. Of these the most interesting is because it exhibits a large hyperfine... [Pg.746]

The negative entries above result when the first emd second isotope peaks are more intense than the lowest isotopomer peak. The remedning 6855 spectrum-structure pairs are distributed over another 360 mass differences. Knowledge of this mass... [Pg.312]

The antisymmetric stretching vibration in the electronic ground state X Bi, V3 = 3359.932(2) cm", was obtained from an IR absorption spectrum [1]. Additional vibrational frequencies of NH2 in the three lowest electronic states were determined from photoelectron spectra (PES) of NH2(X Bi) [6]. Vibrational frequencies of NH2 and Isotopomers (in cm" ) from experiments (see data collections [7 to 9]) and ab initio calculations are listed in the following table ... [Pg.243]

Figure 3 Far-infrared spectrum of the ejecta from the star IRC 10216 obtained with the Long-Wavelength Spectrometer on board the Infrared Space Observatory at a resolution of about 100. Most of the lines In this spectrum can be Identified with pure rotational transitions In CO, HCN and their Isotopomers (top arrows). Rotational transitions associated with the lowest vibrational states of HCN are also present (bottom arrows). Reproduced with permission from Cernicharo J, Barlow MJ, Gonzalez-Alfonso et al (1996) Astronomy and Astrophysics 315 L201. Figure 3 Far-infrared spectrum of the ejecta from the star IRC 10216 obtained with the Long-Wavelength Spectrometer on board the Infrared Space Observatory at a resolution of about 100. Most of the lines In this spectrum can be Identified with pure rotational transitions In CO, HCN and their Isotopomers (top arrows). Rotational transitions associated with the lowest vibrational states of HCN are also present (bottom arrows). Reproduced with permission from Cernicharo J, Barlow MJ, Gonzalez-Alfonso et al (1996) Astronomy and Astrophysics 315 L201.

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See also in sourсe #XX -- [ Pg.310 ]




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