High‐Temperature Lines in SUMER Spectra Recorded Above a Bright Solar Active Region

We identify spectral lines emitted by solar abundant elements due primarily to transitions within the 2 s 2 2 p k and 3 s 2 3 p k (where k = 1, 5) ground configurations of ions that are formed in ionization equilibrium between 2 × 10 6 and 8 × 10 6 K. The transitions were identified in spectra of a bright active region recorded 1997 September 6, by the Solar Ultraviolet Measurements of Emitted Radiation Spectrometer (SUMER) flown on the Solar and Heliospheric Observatory ( SOHO ). Some of these lines provide useful plasma diagnostic tools for measuring the physical conditions in the solar corona.