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To understand the nature of supernovae and neutron star (NS) formation, aswell as binary stellar evolution and their interactions, it is important toprobe the distribution of NS masses. Until now, all double NS (DNS) systemshave been measured to have a mass ratio close to unity (q $\geq$ 0.91). Here wereport the measurement of the individual masses of the 4.07-day binary pulsarJ0453+1559 from measurements of the rate of advance of periastron and Shapirodelay: The mass of the pulsar is 1.559(5) $M_{\odot}$ and that of its companionis 1.174(4) $M_{\odot}$; q = 0.75. If this companion is also a neutron star(NS), as indicated by the orbital eccentricity of the system (e=0.11), then itsmass is the smallest precisely measured for any such object. The pulsar has aspin period of 45.7 ms and a spin derivative of 1.8616(7) x$10^-19$; from thesewe derive a characteristic age of ~ 4.1 x $10^9$ years and a magnetic field of~ 2.9 x $10^9$ G,i.e, this pulsar was mildly recycled by accretion of matterfrom the progenitor of the companion star. This suggests that it was formedwith (very approximately) its current mass. Thus NSs form with a wide range ofmasses, which is important for understanding their formation in supernovae. Itis also important for the search for gravitational waves released during aNS-NS merger: it is now evident that we should not assume all DNS systems aresymmetric.

Pulsar J0453+1559: A Double Neutron Star System with a Large Mass Asymmetry