DOI: 10.6084/m9.figshare.1012704.v1
title: Analysis of the 6.0 GHz He I spectrum from Orion A [8]

description: <b>Table 9.</b> Analysis of the 6.0 GHz He I spectrum from Orion A [8]. The columns and their headings (symbols) correspond to those in tables 5–8, except that the line strengths and thus relative intensities are twice the corresponding values for H I under identical conditions. In this case, the frequency of the leading (most intense) member of the series is <em>f</em><sub>0</sub> = 6.109 34 GHz. As in the other tables, a quantity in parentheses indicates the power of 10 by which the corresponding entry should be multiplied. <strong>Abstract</strong> Since highly excited atoms, which contribute to the radio recombination spectra from Galactic H II regions, possess large polarizabilities, their lifetimes are influenced by ion (proton)–induced dipole collisions. It is shown that, while these ion–radiator collisional processes, if acting alone, would effectively limit the upper principal quantum number attainable for given plasma parameters, their influence is small relative to that of electron impacts within the framework of line broadening theory. The present work suggests that ion–permanent dipole interactions (Hey <em>et al</em> 2004 <em>J. Phys. B: At. Mol. Opt. Phys.</em> <strong>37</strong> 2543) would also be of minor importance in limiting the occupation of highly excited states. On the other hand, the ion–induced dipole collisions are essential for ensuring equipartition of energy between atomic and electron kinetic distributions (Hey <em>et al</em> 1999 <em>J. Phys. B: At. Mol. Opt. Phys.</em> <strong>32</strong> 3555; 2005 <em>J. Phys. B: At. Mol. Opt. Phys.</em> <strong>38</strong> 3517), without which Voigt profile analysis to extract impact broadening widths would not be possible. Electron densities deduced from electron impact broadening of individual lines (Griem 1967 <em>Astrophys. J.</em> <strong>148</strong> 547; Watson 2006 <em>J. Phys. B: At. Mol. Opt. Phys.</em> <strong>39</strong> 1889) may be used to check the significance of the constraints arising from the present analysis. The spectra of Bell <em>et al</em> (2000 <em>Publ. Astron. Soc. Pac.</em> <strong>112</strong> 1236; 2011 <em>Astrophys. Space Sci</em>. <strong>333</strong> 377; 2011 <em>Astrophys. Space Sci</em>. <strong>335</strong> 451) for Orion A and W51 in the vicinity of 6.0 and 17.6 GHz are examined in this context, and also in terms of a possible role of the background ion microfield in reducing the near-elastic contributions to the electron impact broadening below the predictions of theory (Hey 2012 <em>J. Phys. B: At. Mol. Opt. Phys.</em> <strong>45</strong> 065701). These spectra are analysed, subject to the constraint that calculated relative intensities of lines, arising from upper states in collisional–radiative equilibrium, should be consistent with those obtained from Voigt profile analysis. It is shown that the experimental technique yields an excellent temperature diagnostic for the H II regions. On the other hand, strong evidence is not obtained, from those spectra which satisfy the above constraint on intensity, to indicate that the electron impact broadening theory requires substantial correction. The main grounds for attempting a revision of theory to allow for the influence of the ion microfield during the scattering processes on the upper and lower states of each line thus still appear to have a stronger theoretical (Hey 2007 <em>J. Phys. B: At. Mol. Opt. Phys.</em> <strong>40</strong> 4077) than experimental basis.