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The interpretation of microlensing results towards the Large  Magellanic Cloud (LMC) still remains controversial. White dwarfs have beenproposed to explain these results and, hence, to contribute significantly tothe mass budget of our Galaxy. However, several constraints on the role playedby regular carbon-oxygen white dwarfs exist. Massivewhite dwarfs are thought tobe made of a mixture of oxygen and neon. Correspondingly, their cooling rate islarger than those of typical carbon-oxygen white dwarfs and they fade toinvisibility in short timescales. Consequently, they constitute a goodcandidate for explaining the microlensing results. Here, we examine in detailthis hypothesis by using the most recent and up-to-date cooling tracks formassive white dwarfs and a Monte Carlo simulator which takes into account themost relevant Galactic inputs. We find that oxygen-neon white dwarfs cannotaccount for a substantial fraction of the microlensing depth towards the LMC,independently of the adopted initial mass function, although some microlensingevents could be due to oxygen--neon white dwarfs. The white dwarf populationcontributes at most a 5% to the mass of the Galactic halo.

The contribution of Oxygen-Neon white dwarfs to the MACHO content of the Galactic Halo