Titlebook: Iron Line Diagnostics in X-ray Sources; Proceedings of a Wor A. Treves,G. C. Perola,L. Stella Conference proceedings 1991 Springer-Verlag B

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Iron L-shell line formation in diverse astrophysical environments,rse astronomical sources. Although few data sets of adequate statistical quality are currently available for analysis, the next series of X-ray satellite experiments will provide order-of-magnitude improvements in both resolution and sensitivity for this kind of work. We review the important physica

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X-ray lines in stellar coronae,ous application in the measurement of optically thin sources such as the coronae of stars. In particular X-ray observations with the . observatory have demonstrated that soft X-ray emitting coronae are a common feature among stars on the cool side of the Hertzsprung-Russell diagram, with the probabl

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GINGA observations of AB Doradus,be present. four X-ray flares were detected. Three of these events were similar to the . HRI-flare (Vilhu and Linsky, 1987), with decay times around 25 min. The last flare had long rise and decay times (100 min), resembling the . flares observed by Collier Cameron et.al. (1988). The mean flare spect

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SPARTAN 1 X-ray observation of diffuse emission at the galactic center, and extended emission ~1. In diameter centered near the galactic center were detected [1]. We have re-analyzed the diffuse component data following the discovery [2] of Intense Fe line emission. The radial distribution of this component Is examined by grouping the data Into radial bins centered on

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Iron line diagnostics in elliptical galaxies and cluster cooling flows,uch of this gas has probably come out of stars and been ejected from galaxies in the cluster. In elliptical galaxies, iron and other X-ray lines can establish whether the X-ray emission is due to diffuse thermal emission, which is particularly uncertain for the fainter galaxies. X-ray line observati

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,The distribution of iron in galaxy clusters — results from the spacelab 2 X-ray telescope,y band of the telescope encompasses the iron K complex, so that the spatial distribution of the iron line emission can be mapped. Here we present results for the distribution of iron abundance which can be inferred in the three brightest X-ray clusters: Perseus, Coma and Ophiuchus.

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