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Methanol (CH$_3$OH) is found to be abundant and widespread towards theCentral Molecular Zone, the inner few hundred parsecs of our Galaxy. Its originis, however, not fully understood. It was proposed that the high cosmic rayionisation rate in this region could lead to a more efficient non-thermaldesorption of this species formed on grain surfaces, but it would also meanthat this species is destroyed in a relatively short timescale. In a firststep, we run chemical models with a high cosmic ray ionisation rate and findthat this scenario can only reproduce the lowest abundances of methanol derivedin this region ($\sim$10$^{-9}$-10$^{-8}$). In a second step, we investigateanother scenario based on episodic explosions of grain mantles. We find a goodagreement between the predicted abundances of methanol and the observations. Wefind that the dominant route for the formation of methanol is throughhydrogenation of CO on the grains followed by the desorption due to the grainmantle explosion. The cyclic aspect of this model can explain the widespreadpresence of methanol without requiring any additional mechanism. We also modelsilicon monoxide (SiO), another species detected in several molecular clouds ofthe Galactic Centre. An agreement is found with observations for a highdepletion of Si (Si/H $\sim$ 10$^{-8}$) with respect to the solar abundance.

A study of methanol and silicon monoxide production through episodic explosions of grain mantles in the Central Molecular Zone