# First Application of the Fe XVII I(17.10 A)/I(17.05 A) Line Ratio to Constrain the Plasma Density of a Cosmic X-ray Source Source: [First Application of the Fe XVII I(17.10 A)/I(17.05 A) Line Ratio to Constrain the Plasma Density of a Cosmic X-ray Source]() Collection index: [llms.txt]() Data updated: 2025-10-24T10:36:49.910Z Authors: Christopher W. Mauche, Duane A. Liedahl, Kevin B. Fournier Published: 2001-06-28T00:27:09.000Z ## Abstract We show that the Fe XVII I(17.10 A)/I(17.05 A) line ratio observed in the Chandra HETG spectrum of the intermediate polar EX Hydrae is significantly smaller than that observed in the Sun or other late-type stars. Using the Livermore X-ray Spectral Synthesizer, which calculates spectral models of highly charged ions based on HULLAC atomic data, we find that the observed I(17.10 A)/I(17.05 A) line ratio can be explained if the plasma density n\_e \> 3x10^{14} cm^{-3}. However, if photoexcitation is included in the level population kinetics, the line ratio can be explained for any density if the photoexcitation temperature T\_bb \> 55 kK. For photoexcitation to dominate the Fe XVII level population kinetics, the relative size of the hotspot on the white dwarf surface must be f \< 2%. This constraint and the observed X-ray flux requires a density n \> 2x10^{14} cm^{-3} for the post-shock flow. Either way, then, the Chandra HETG spectrum of EX Hya requires a plasma density which is orders of magnitude greater than that observed in the Sun or other late-type stars. ## Recorded benchmark results A research result applies to its stated dataset, split, metric and evaluation configuration. Compare like-for-like settings, preserve the metric's unit and direction, and distinguish paper-reported results from independent reproduction. The best result recorded here is not a claim of exhaustive, current global coverage. ## Original sources and implementation [Original paper]() [PDF]()