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We analyze binary population models of double-neutron stars and compareresults to the accurately measured orbital periods and eccentricities of theeight known such systems in our Galaxy. In contrast to past similar studies, weespecially focus on the dominant evolutionary channels (we identify three); forthe first time, we use a detailed understanding of the evolutionary history ofthree double neutron stars as actual constraints on the population models. Wefind that the evolutionary constraints derived from the double pulsar areparticularly tight, and less than half of the examined models survive the fullset of constraints. The top-likelihood surviving models yield constraints onthe key binary evolution parameters, but most interestingly reveal (i) the needfor electron-capture supernovae from relatively low-mass degenerate, progenitorcores, and (ii) the most likely evolutionary paths for the rest of the knowndouble neutron stars. In particular, we find that J1913+16 likely went througha phase of Case BB mass transfer, and J1906+0746 and J1756-2251 are consistentwith having been formed in electron-capture supernovae.

Evolutionary Channels for the Formation of Double Neutron Stars