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Type-I X-ray bursts are thermonuclear explosions occurring in the surfacelayers of accreting neutron stars. These events are powerful probes of thephysics of neutron stars and their surrounding accretion flow. We analyze avery energetic type-I X-ray burst from the neutron star low-mass X-ray binaryIGR J17062-6143 that was detected with Swift on 2012 June 25. The light curveof the ~18 min long X-ray burst tail shows an episode of ~10 min during whichthe intensity is strongly fluctuating by a factor of ~3 above and below theunderlying decay trend, on a time scale of seconds. The X-ray spectrum revealsa highly significant emission line around ~1 keV, which can be interpreted as aFe-L shell line caused by irradiation of cold gas. We also detect significantabsorption lines and edges in the Fe-K band, which are strongly suggestive ofthe presence of hot, highly ionized gas along the line of sight. None of thesefeatures are present in the persistent X-ray spectrum of the source. The timescale of the strong intensity variations, the velocity width of the Fe-Lemission line (assuming Keplerian motion), and photoionization modeling of theFe-K absorption features each independently point to gas at a radius of ~1E3 kmas the source of these features. The unusual X-ray light curve and spectralproperties could have plausibly been caused by a disruption of the accretiondisk due to the super-Eddington fluxes reached during the X-ray burst.

X-ray emission and absorption features during an energetic thermonuclear X-ray burst from IGR J17062-6143