Abstract
We present results of a population synthesis study aimed at examining the role of spin‐kick alignment in producing a correlation between the spin period of the first‐born neutron star and the orbital eccentricity of observed double neutron star binaries in the Galactic disk. We find spin‐kick alignment to be compatible with the observed correlation, but not to alleviate the requirements for low kick velocities suggested in previous population synthesis studies. Our results furthermore suggest low‐ and high‐eccentricity systems may form through two distinct formation channels distinguished by the presence or absence of a stable mass transfer phase before the formation of the second neutron star. The presence of highly eccentric systems in the observed sample of double neutron stars may furthermore support the notion that neutron stars accrete matter when moving through the envelope of a giant companion.
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