Identification of spectral lines in the 500-1600 angstrom wavelength rangeof highly ionized Ne, Na, Mg, Ar, K, Ca, Ti, Cr, Mn, Fe, Co, and Ni emitted by flares (T-e >= 3 x 10(6) K) and their potential use in plasma diagnostics

On 1999 May 9 the Solar Ultraviolet Measurements of Emitted Radiation (SUME R) spectrometer on the Solar and Heliospheric Observatory (SOHO) recorded s pectra 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-temp erature (T-e greater than or equal to 3 x 10(6) K) Ne, Na, Mg, Ar, K, Ca, T i, Cr, Mn, Fe, Co, and Ni lines that were detected in the 500-1600 Angstrom spectral range of SUMER. In addition, accurate wavelength measurements hav e 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 p resent 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 th at could be used to determine emission measures and electron temperatures o f high-temperature plasmas. We discuss a method for measuring elemental abu ndance variations in high-temperature solar plasmas using lines presented i n the paper. A list of spectral lines spanning the 300-30000 Angstrom wavel ength range and their branching ratios that are suitable for efficiency cal ibration of space-borne spectrographs is provided.