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Abstract:
To gain insight into the stellar evolution of stars one can use the astronomical observations
of elements that are heavier than iron. The atomic data of such elements
are necessary in order to interpret stars’ spectroscopic observations. Technetium
(Z=43) is of particular interest since it is the lightest element with no stable isotopes
and it has a limited lifetime. Observation of such element from the stars can
provide a time scale of their evolutionary stages. Very similar to Technetium in its
electronic structure is Ruthenium (Z=44), which in this thesis will be used to assign
the observed lines of this element to their possible charge state. These lines were
measured using an electron beam ion trap at the Max Planck Institute for Nuclear
Physics in Heidelberg. Through a flat-field grazing incidence spectrometer florescent
light from excited ruthenium ions, in the 17–27nm wavelength range, was recorded.
Considering the intensity of different spectral lines at different electron beam energies,
the presence of metastable states could be observed. The contributions of
metastable states were discussed using three different approaches where the space
charge potential of the electron beam was corrected differently.
