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We search for EUV brightenings in TRACE 171 {\AA} images and HXR burstsobserved during failed eruptions. We expect that if an eruption is confined dueto interaction with overlying magnetic structures then we should observeeffects connected with reconnection between magnetic structures andacceleration of particles. We utilized TRACE observations of three wellobserved failed eruptions. EUV images were compared to HXR spatial distributionreconstructed from Yohkoh/HXT and RHESSI data. The EUV light curves of aselected area were compared to height profiles of eruption, HXR emission andHXR photon spectral index of power-law fit to HXR data. We have found that EUVbrightenings are closely related to the eruption velocity decrease, to HXRbursts and to episodes of hardening of HXR spectra. The EUV brightened areasare observed far from the flaring structure, in footpoints of large systems ofloops observed 30-60 minutes after the maximum of a flare. These are not`post-flare' loops that are also observed but at significantly lower heights.The high lying systems of loops are observed at heights equal to height, atwhich eruption was observed to stop. We observed HXR source spatiallycorrelated with EUV brightening only once. For other EUV brightened areas weestimated the expected brightness of HXR sources. We find that EUV brighteningsare produced due to interaction between the erupting structure with overlyingloops. The interaction is strong enough to heat the system of high loops. Theseloops cool down and are visible in EUV range about 30-60 minutes later. Theestimated brightness of HXR sources associated with EUV brightenings shows thatthey are too weak to be detected with present instruments. However, nextgeneration instruments will have enough dynamic range and sensitivity to enablesuch observations.

EUV and HXR Signatures of Electron Acceleration During the Failed Eruption of a Filament