First detection of relativistic angular deformation δ_θ in PSR J1757−1854 via MeerKAT-enhanced timing, ruling out two of four prior geometric solutions while confirming GR consistency for orbital decay.
The Masses of Two Binary Neutron Star Systems
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abstract
The measurement or constraint of the masses of neutron stars and their binary companions tests theories of neutron star structure and of pulsar formation and evolution. We have measured the rate of the general relativistic advance of the longitude of periastron for the pulsar PSR B1802$-$07: $\dot\omega=0\fdg060\pm0\fdg009\,\mbox{yr}^{-1}$, which implies a total system mass, pulsar plus companion star, of $M=1.7\pm0.4\,\Msun$. We also present a much improved measurement of the rate of periastron advance for PSR B2303+46: $\dot\omega = 0\fdg0099\pm0\fdg0002\,\mbox{yr}^{-1}$, implying $M=2.53\pm0.08\,\Msun$ for this system. We discuss the available constraints on distribution of mass between the pulsars and their companions, and we compare the pulsar masses with other determinations of neutron star masses.
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Detection of relativistic orbital deformation from improved timing of PSR J1757$-$1854
First detection of relativistic angular deformation δ_θ in PSR J1757−1854 via MeerKAT-enhanced timing, ruling out two of four prior geometric solutions while confirming GR consistency for orbital decay.