LαSatellite Lines for Elements Mo(42) to Ba(56)

The x-ray satellite lines accompanying the $L{\alpha }_{1,2}$ emission for elements Mo(42) to Ba(56) have been systematically studied with a two-crystal vacuum spectrometer. Integrated relative intensities of the satellite group agree qualitatively but differ by a factor of about six with previous photographic measurements. The abrupt intensity change at $Z=50\mathrm{}$ (the element at which the Coster-Kronig "cross-over" occurs) further confirms qualitatively the Coster-Kronig interpretation of Auger production of the initial state in satellite emission. The observed satellite contour for each element has been resolved arbitrarily into constituent component lines and wave-lengths and relative intensities measured. A few hitherto unreported satellite components are found: Theory predicts fifteen $L\alpha$ satellite components for Au(79), about twice as many as are included in the present analyses for the intermediate atomic numbers. The components farthest removed from the $L{\alpha }_1$ line seem not to exhibit the abrupt intensity change at $Z=50\mathrm{}$ and, therefore, may not be from the $L_{\mathrm{III}}{M}_{\mathrm{I}\mathrm{V},\mathrm{V}}$ initial state. These components may be Wentzel-Druyvesteyn satellites from another initial state or they may be Richtmyer satellites.