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Abstract: Multiband observations show clear evidence for large-scale magnetic interaction of coronal loops in solar active regions. These loops are transiently (~20 min) bright in hot EUV channels (Atmospheric Imaging Assembly on-board Solar Dynamics Observatory, SDO/AIA), with temperatures up to about 10 MK, intersect in the plane of the sky, and their footpoints are hot spots for a short time in transition region UV lines (Interface Region Imaging Spectrograph, IRIS). The UV spectral features can be explained as produced by non-thermal electron beams hitting the transition region and generating a heat pulse of less than 1 minute. This is consistent with periodic pulsations detected in EUV light curves along the interacting loops, produced by sloshing wave fronts driven by short heat pulses. These loop systems represent excellent laboratories for studying impulsive heating mechanisms and allow us to focus physical models for diagnostics. We show preliminary MHD modeling of interacting loops.