Magnetic field restructuring by reconnection is pervasive in in solar physics. It can potentially provide the energy to heat and accelerate the plasma in the solar atmosphere. We will investigate the role of small-scale magnetic reconnection in the formation of transition region explosive events. These events are defined by strong transient enhancements of the wings of spectral lines that form at transition region temperatures (between 2 x 10^4 - 2 x 10^5 K). Using SUMER data we are able to identify explosive events by their spectral signature. With MDI we can continuously map the photospheric magnetic field and search for a manifestation of the reconnection in the lower solar atmosphere. We have analysed a number of explosive events and will show how the underlying magnetic field evolves during these events.