XMM-Newton RGS spectrum of the flare star EQ Pegasi
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Image courtesy of J. Schmitt, Hamburger Sternwarte, Germany and ESA.
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About this Image
The spectral lines visible all arise from six times ionized oxygen, which is formed in plasmas of temperatures of 4 million degrees and higher. One recognises three lines at 21.6 Angstrom, the so-called resonance line, at 21.8 Angstrom, the so-called intercombination line, and at 22.1 Angstrom, the so-called forbidden line. The important quantity in this case is the ratio between the line strengths of the forbidden and intercombination lines. In the case of EQ Peg this ratio is found to be 3.2, which indicates that the density of the plasma is relatively large, much larger than the density of the solar corona.
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