Identification of spectral lines in the 500-1600 Å wavelength range of highly ionized Ne, Na, Mg, Ar, K, Ca, Ti, Cr, Mn, Fe, Co, and Ni emitted by flares (Te ≥ 3 x 106 K) and their potential use in plasma diagnostics

On 1999 May 9 the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) spectrometer on the Solar and Heliospheric Observatory (SOHO) recorded spectra from a high-temperature region located in the solar corona above the west limb. These spectra contain lines from rather less-abundant elements in solar plasmas. In this paper we present identifications of the high-temperature (T-e greater than or equal to 3 x 10(6) K) Ne, Na, Mg, Ar, K, Ca, Ti, Cr, Mn, Fe, Co, and Ni lines that were detected in the 500-1600 Angstrom spectral range of SUMER. In addition, accurate wavelength measurements have been obtained with uncertainties varying between 0.015 and 0.040 Angstrom (1 sigma). Making use of the newly measured wavelengths, we derive energy levels in the ground configuration of a number of highly charged ions. We present intensity ratio calculations of lines in the SUMER range that could be used to measure electron densities in high-temperature solar plasmas. We also provide emissivities for Ca xIII-Ca xv and Fe xvIII-Fe xxIII lines that could be used to determine emission measures and electron temperatures of high-temperature plasmas. We discuss a method for measuring elemental abundance variations in high-temperature solar plasmas using lines presented in the paper. A list of spectral lines spanning the 300-30000 Angstrom wavelength range and their branching ratios that are suitable for efficiency calibration of space-borne spectrographs is provided.