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We present a model that explains the anomalous intensity ratios betweeneach of two very bright UV lines of Fe II at 2507 Å and 2509Å and its corresponding satellite line, observed in HST spectra ofa compact gaseous condensation (blob B) in the vicinity of the starprotect eta Car.The model is based on the assumption that the FeIItransitions have a substantial optical thickness, which varies as ares
