Journal
ASTROPHYSICAL JOURNAL
Volume 617, Issue 2, Pages L135-L138Publisher
IOP PUBLISHING LTD
DOI: 10.1086/427235
Keywords
gravitation; pulsars : individual (PSR J0737-3039); stars : neutron; stars : rotation
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We construct numerical models of the newly discovered binary pulsar J0737-3039A, both with a fully relativistic, uniformly rotating equilibrium code that handles arbitrary spins and in the relativistic slow-rotation approximation. We compare results for a representative sample of viable nuclear equations of state (EOSs) that span three qualitatively different classes of models for the description of nuclear matter. A future dynamical measurement of the neutron star's moment of inertia from pulsar timing data will impose significant constraints on the nuclear EOS. Even a moderately accurate measurement (less than or similar to10%) may be able to rule out some of these competing classes. Using the measured mass, spin, and moment of inertia to identify the optimal model computed from different EOSs, one can determine the pulsar's radius.
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