Observations of a number of helium triplet (~.210830, 4713, 4471, 3889, 4026) and hydrogea (H),, g, r/, 0) emission line intensities in six quiescent prominences are presented. The regions of prominence and neighboring corona were raster-scanned by the telescope, and all lines were measured concurrently at each point. The instrumental field of view was 5" • 20". The results are compared with previous observations and theory. In particular, the intensity of the 210830 emission relative to the other triplets is found to differ strongly from the predictions of the recent detailed calculations of Heasley et al. (1974) for model quiescent prominences.
2By means of the atomic-beammagnetic-resonance method we have measured the P3/2 level hfs and the P3/2 and P&~2 level gz factors of the Bi (6p) ground configuration. Our experimental results are: A( P3/2) =491.028(1) MHz, B( P3/2) = 978.639(9) MHz, C( P3/2) = 0.0193(5) MHz, g~( P&&2) = 0.6654(2) and g&( P3/2) =1.26083(12). In order to interpret these measurements, we have examined the fine structure and the hfs of all the (6p) levels. Our calculations show that the inclusion of spin-spin, orbit-orbit, and spin-other-orbit interactions do not improve the theoretical fit to the observed fine structure intervals. The effects of core polarization and relativity can be estimated by writing the dipole hfs Hamiltonian in the form Z=2p)gsI'g; [(r& );f;v"10 (r c);(sC); + (r );s;].This analysis of the dipole hfs yields a value (~) +, (hfs) =1.02x10 cm compared to the fine structure result(r )8&(fs) =1.25xl0 cm . With these results we find Q= -0.383(40) b and n = 0.55(3)p,"b.
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