The M dwarf problem: Fe and Ti abundances in a volume-limited sample of M dwarf stars. (arXiv:2003.11447v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Woolf_V/0/1/0/all/0/1">Vincent M .Woolf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wallerstein_G/0/1/0/all/0/1">George Wallerstein</a>
We report iron and titanium abundance measurements from high resolution
spectrain a volume-limited sample of 106 M0 and M0.5 dwarf stars. The sample
includesstars north of the celestial equator and closer than 29 parsecs. The
results imply thatthere is an M dwarf problem similar to the previously known G
dwarf problem, in thatthe fraction of low-metallicity M dwarfs is not large
enough to fit simple closed-boxmodels of Galactic chemical evolution. This
volume-limited sample avoids many of thestatistical uncertainties present in a
previous study using a brightness-limited sampleof M dwarf stars
We report iron and titanium abundance measurements from high resolution
spectrain a volume-limited sample of 106 M0 and M0.5 dwarf stars. The sample
includesstars north of the celestial equator and closer than 29 parsecs. The
results imply thatthere is an M dwarf problem similar to the previously known G
dwarf problem, in thatthe fraction of low-metallicity M dwarfs is not large
enough to fit simple closed-boxmodels of Galactic chemical evolution. This
volume-limited sample avoids many of thestatistical uncertainties present in a
previous study using a brightness-limited sampleof M dwarf stars
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