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Theoretical stellar evolution models are constructed and tailored to the bestknown, observationally derived characteristics of metal-poor ([Fe/H]$\sim-2.3$)stars representing a range of evolutionary phases: subgiant HD140283, globularcluster M92, and four single, main sequence stars with well-determinedparallaxes: HIP46120, HIP54639, HIP106924, and WOLF1137. It is found that theuse of a solar-calibrated value of the mixing length parameter$\alpha_{\text{MLT}}$ in models of these objects is ineffective at reproducingtheir observed properties. Empirically calibrated values of$\alpha_{\text{MLT}}$ are presented for each object, accounting foruncertainties in the input physics employed in the models. It is advocated thatthe implementation of an adaptive mixing length is necessary in order forstellar evolution models to maintain fidelity in the era of asteroseismicobservations.

Not All Stars Are the Sun: Empirical Calibration of the Mixing Length for Metal-Poor Stars Using One-dimensional Stellar Evolution Models