Constraining the gravitational binding energy of PSR J0737-3039B using terrestrial nuclear data

Abstract

We show that the gravitational binding energy of a neutron star of a given mass is correlated with the slope of the nuclear symmetry energy at 1-2 times nuclear saturation density for equations of state without significant softening (i.e., those that predict maximum masses $M_{\max }>1.44M_{\odot }$ in line with the largest accurately measured neutron star mass). Applying recent laboratory constraints on the slope of the symmetry energy to this correlation we extract a constraint on the baryon mass of the lower mass member of the double pulsar binary system, PSR J0737-3039B. We compare with independent constraints derived from modeling the progenitor star of J0737-3039B up to and through its collapse under the assumption that it formed in an electron capture supernova. The two sets of constraints are consistent only if $L\lesssim$ 70 MeV.

18 pages, 4 figures

References in corpus (6)

• Nuclear symmetry energy probed by neutron skin thickness of nuclei
• Cold uniform matter and neutron stars in the quark-mesons-coupling model
• Isospin-dependent properties of asymmetric nuclear matter in relativistic mean-field models
• The Formation of the Double Pulsar PSR J0737-3039A/B
• The double pulsar: evolutionary constraints from the system geometry
• Symmetry Energy as a Function of Density and Mass

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