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

Details 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 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

2001-06-28

arxiv.org/abs/astro-ph/0106518v1

Astronomy and Astrophysics

Astrophysics

13 pages including 1 table and 4 encapsulated postscript figures; LaTeX format, uses aastex.cls; accepted on 2001 June 27 for

Scientific paper

10.1086/323067

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.

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