Abstract
We observed the X‐ray afterglow of GRB 970828 with the Japanese X‐ray satellite ASCA. The spectral data displayed a hump around ∼ 5 keV. This hump structure is likely a recombination edge of iron in the vicinity of the source, taking into account the redshift z = 0.9578 found for the likely host galaxy of the associated radio flare. The Radiative Recombination Edge and Continuum model can interpret the spectrum as coming from a highly ionized plasma in a non‐equilibrium ionization state.
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