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The rich open cluster M67 is known to have a chemical composition close tosolar, and an age around 4Gyr. It thus offers the opportunity to check ourunderstanding of the physics and the evolution of solar-type stars in a clusterenvironment. We present the first spectroscopic study at high resolution,R~50,000, of the potentially best solar twin, M67-1194, identified amongsolar-like stars in M67. Based on a pre-selection of solar-twin candidatesperformed at medium resolution by Pasquini et al. (2008), we explore thechemical-abundance similarities and differences between M67-1194 and the Sun,using VLT/FLAMES-UVES. Working with a solar twin in the framework of adifferential analysis, we minimize systematic model errors in the abundanceanalysis compared to previous studies which utilized more evolved stars todetermine the metallicity of M67. We find M67-1194 to have stellar parametersindistinguishable from the solar values, with the exception of the overallmetallicity which is slightly super-solar ([Fe/H]=0.023 +/- 0.015). An agedetermination based on evolutionary tracks yields 4.2 +/- 1.6Gyr. Mostsurprisingly, we find the chemical abundance pattern to closely resemble thesolar one, in contrast to most known solar twins in the solar neighbourhood. Weconfirm the solar-twin nature of M67-1194, the first solar twin known to belongto a stellar association. This fact allows us to put some constraints on thephysical reasons for the seemingly systematic departure of M67-1194 and the Sunfrom most known solar twins regarding chemical composition. We find thatradiative dust cleansing by nearby luminous stars may be the explanation forthe peculiar composition of both the Sun and M67-1194, but alternativeexplanations are also possible. The chemical similarity between the Sun andM67-1194 also suggests that the Sun once formed in a cluster like M67.

M67-1194, an unusually Sun-like solar twin in M67