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The Fe Kα lines in gamma-ray bursts (GRBs) produced with the Cerenkov line mechan ism are studied. We theoretically predict the Fe Kα line luminosities in both the early (before 1 hour) and late (～ 1 day) afterglows. Assuming about 200 GRBs could be detected by Swift per year, we sampled the redshift of these GRBs using the Monte Carlo method according to the GRB formation rate derived from the statistical correlation between the spectral peak energy and the peak luminosity of GRBs.