Observations of the iron emission lines in the X-ray spectrum of the supernova remnant Cassiopeia A

Details Observations of the iron emission lines in the X-ray spectrum of the supernova remnant Cassiopeia A Observations of the iron emission lines in the X-ray spectrum of the supernova remnant Cassiopeia A

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...122..124m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 122, no. 1-2, June 1983, p. 124-128.

Astronomy and Astrophysics

Astrophysics

5

Emission Spectra, Iron, Line Spectra, Stellar Spectrophotometry, Supernova Remnants, X Ray Spectra, Abundance, High Temperature Plasmas, Scintillation Counters, Spectral Line Width, Stellar Envelopes, Stellar Evolution

Scientific paper

Observations of the X-ray spectrum of the supernova remnant Cassiopeia A over the energy range 2-10 keV are presented. The results, obtained by the use of two gas scintillation proportional counter spectrometers flown on an Aries rocket confirm the presence of a strong blend of emissions lines between 6.5-7.5 keV. The principal line in the blend is tentatively considered to result from the 1s-2p transition in Hydrogen-like iron, Fe XXVI. The equivalent width of the blend is found to be 952 ± 143 eV consistent with the previous observations made with conventional proportional counters. Evidence for a weaker blend probably from the 1s-3p transition in Fe XXVI is also found. This transition, which can be clearly resolved by the spectrometer from the stronger blend has an equivalent width of 434 ± 102 eV. If the line emission does result primarily from transitions in hydrogenic iron then a significant component of the high temperature plasma associated with the shocked circumstellar material must be at temperatures above 1.5 108 K.

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