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[Abridged] Ethylene oxide and its isomer acetaldehyde are important complexorganic molecules because of their potential role in the formation of aminoacids. Despite the fact that acetaldehyde is ubiquitous in the interstellarmedium, ethylene oxide has not yet been detected in cold sources. We aim tounderstand the chemistry of the formation and loss of ethylene oxide in hot andcold interstellar objects (i) by including in a revised gas-grain network somerecent experimental results on grain surfaces and (ii) by comparison with thechemical behaviour of its isomer, acetaldehyde. We test the code for the caseof a hot core. The model allows us to predict the gaseous and solid ethyleneoxide abundances during a cooling-down phase prior to star formation and duringthe subsequent warm-up phase. We can therefore predict at what temperaturesethylene oxide forms on grain surfaces and at what temperature it starts todesorb into the gas phase. The model reproduces the observed gaseous abundancesof ethylene oxide and acetaldehyde towards high-mass star-forming regions. Inaddition, our results show that ethylene oxide may be present in outer andcooler regions of hot cores where its isomer has already been detected. Despitetheir different chemical structures, the chemistry of ethylene oxide is coupledto that of acetaldehyde, suggesting that acetaldehyde may be used as a tracerfor ethylene oxide towards cold cores.

Ethylene oxide and Acetaldehyde in hot cores