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Abstract:
In this work, the following transitions are spectroscopically investigated: Fe13+ at 530 nm,
Fe9+ at 637 nm, Fe12+ at 339 nm and Fe10+ at 789 nm. These transitions occur in the solar
corona and other stars and are therefore of astrophysical interest. Reference wavelength
values are needed to determine plasma movements and temperatures in those stars, but scarce
laboratory measurements are available and theoretical calculations are not sufficiently precise.
In our case, those highly charged ions are produced in the laboratory using an electron beam
ion trap. The wavelengths and g-factors are determined: 530.42870(8) nm, 637.6277(4) nm,
338.8930(3) nm, 789.3915(8) nm. For the Fe13+ at 530 nm, Fe9+ at 637 nm and Fe10+ at 789
nm transitions, the Zeeman components are well resolved. For all the measured wavelength,
the uncertainty is 5-14 times smaller than for the previous best measurement.
