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We report iron and titanium abundance measurements from high resolutionspectra in a volume-limited sample of 106 M0 and M0.5 dwarf stars. The sampleincludes stars north of the celestial equator and closer than 29 parsecs. Theresults imply that there is an M dwarf problem similar to the previously knownG dwarf problem, in that the fraction of low-metallicity M dwarfs is not largeenough to fit simple closed-box models of Galactic chemical evolution. Thisvolume-limited sample avoids many of the statistical uncertainties present in aprevious study using a brightness-limited sample of M dwarf stars

The M dwarf problem: Fe and Ti abundances in a volume-limited sample of M dwarf stars