The question "can observations of masses (M's) and radii (R's) of several individual neutron stars uniquely determine the dense matter equation of state (EOS)?" is addressed. By exploiting the one-to-one correspondence between an EOS and the M-R curve generated through the use of the Tolman-Oppenheimer-Volkov equations of stellar structure, we have devised an inversion procedure that can generate the pressure-density relationship once several M's and R's of individual stars are available. The results of this program promises to provide a benchmark model-independent EOS for on-going microscopic studies to shoot for.
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