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The progenitor systems and explosion mechanisms responsible for thethermonuclear events observationally classified as Type Ia supernovae areuncertain and difficult to uniquely constrain using traditional observations ofType Ia supernova host galaxies, progenitors, light curves, and remnants. Forthe subset of thermonuclear events that are prolific producers of iron, we usepublished theoretical nucleosynthetic yields to identify a set of elementalabundance ratios infrequently observed in metal-poor stars but shared across arange of progenitor systems and explosion mechanisms: [Na,Mg,Co/Fe]<0. We labelstars with this abundance signature ``iron-rich metal-poor'' or IRMP stars. Wesuggest that IRMP stars formed in environments dominated by thermonuclearnucleosynthesis and consequently that their elemental abundances can be used toconstrain both the progenitor systems and explosion mechanisms responsible forthermonuclear explosions. We identify three IRMP in the literature andhomogeneously infer their elemental abundances. We find that the elementalabundances of BD+80 245, HE 0533--5340, and SMSS J034249.53--284216.0 are bestexplained by the (double) detonations of sub-Chandrasekhar mass CO whitedwarfs. If our interpretation of IRMP stars is accurate, then they should bevery rare in globular clusters and more common in the Magellanic Clouds anddwarf spheroidal galaxies than in the Milky Way's halo. We propose that futurestudies of IRMP stars will quantify the relative occurrences of differentthermonuclear event progenitor systems and explosion mechanisms.

Iron-rich Metal-poor Stars and the Astrophysics of Thermonuclear Events  Observationally Classified as Type Ia Supernovae. I. Establishing the  Connection