Observations of highly-ionized interstellar iron

Details Observations of highly-ionized interstellar iron Observations of highly-ionized interstellar iron

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984nascp2345..189h&link_type=abstract

In NASA. Goddard Space Flight Center Local Interstellar Medium, No. 81 p 189-193 (SEE N85-15539 06-90)

Physics

1

Interstellar Gas, Interstellar Matter, Iron, Kinematics, Stellar Luminosity, Stellar Spectra, Background Radiation, Solar Corona, Stellar Temperature, Thermal Emission, X Rays

Scientific paper

The spectra of 24 stars have been observed in the regions of the coronal [Fe X] λ6375 and [Fe XIV] λ5303 lines at detection limits near an equivalent width of 1 mÅ in the best cases. In general agreement with predictions based on a multi-phase model of the interstellar medium, no absorption which can be attributed to Fe X or Fe XIV ions in hot interstellar gas emitting the soft X-ray background is seen in any of these spectra, except for two. Toward λ Cephei an absorption line near λ6375 is measured with an equivalent width of 8.1±2 mÅ, a width corresponding to 20±5 km s-1 or a temperature T ≤ (0.5±0.25)×106K, and, if it is caused by Fe X ions, a radial velocity of -355 km s-1. On that hypothesis, the hot interstellar gas constitutes at least 63% of the column density of gas along this light path.

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