Sergey Postnikov

Ohio University, Athens, OH

The Equation of State of Neutron Star Matter from Observational Masses and Radii through the Inversion of TOV Equations


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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