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Diffuse radio emission associated with the intra-cluster medium (ICM) isobserved in a number of merging galaxy clusters. It is currently believed thatin mergers a fraction of the kinetic energy is channeled into non-thermalcomponents, such as turbulence, cosmic rays and magnetic fields, that may leadto the formation of giant synchrotron sources in the ICM. Studying merginggalaxy clusters in different evolutionary phases is fundamental tounderstanding the origin of radio emission in the ICM. We observed the nearbygalaxy cluster pair RXC J1825.3+3026 ($z\sim0.065$) and CIZA J1824.1+3029($z\sim0.071$) at 120-168 MHz with the LOw Frequency ARray (LOFAR) and made useof a deep (240 ks) XMM-Newton dataset to study the non-thermal and thermalproperties of the system. RXC J1825.3+3026 is in a complex dynamical state,with a primary on-going merger in the E-W direction and a secondary later stagemerger with a group of galaxies in the SW, while CIZA J1824.1+3029 isdynamically relaxed. These two clusters are in a pre-merger phase. We reportthe discovery of a Mpc-scale radio halo with a low surface brightness extensionin RXC J1825.3+3026 that follows the X-ray emission from the cluster center tothe remnant of a galaxy group in the SW. This is among the least massivesystems and the faintest giant radio halo known to date. Contrary to this, nodiffuse radio emission is observed in CIZA J1824.1+3029 nor in the regionbetween the pre-merger cluster pair. The power spectra of the X-ray surfacebrightness fluctuations of RXC J1825.3+3026 and CIZA J1824.1+3029 are inagreement with the findings for clusters exhibiting a radio halo and the oneswhere no radio emission has been detected, respectively. We providequantitative support to the idea that cluster mergers play a crucial role inthe generation of non-thermal components in the ICM.

Particle acceleration in a nearby galaxy cluster pair: the role of cluster dynamics