XMM-Newton RGS spectrum of the flare star EQ Pegasi
Minimum credit line: Image courtesy of J. Schmitt, Hamburger Sternwarte, Germany and ESA. (for details, see Conditions of Use).
Credit: ESA/XMM-Newton, CC BY-SA 3.0 IGO
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| About this Image |
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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.
Investigator(s): J. Schmitt
| For More Information |
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- Detailed description of this image
- Query XSA archive for XMM-Newton data in the field of EQ Peg
- Astronomical database entries for EQ Peg;
- Query NED for more images about EQ Peg
- Query SIMBAD for more EQ Peg data
- For unfamiliar terms, visit the XMM-Newton Astronomical Glossary
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