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The recent discovery of a population of eccentric (e ~ 0.1) millisecondpulsar (MSP) binaries with low-mass white dwarf companions in the Galacticfield represents a challenge to evolutionary models that explain MSP formationas recycling: all such models predict that the orbits become highlycircularised during a long period of accretion. The members of this newpopulation exhibit remarkably similar properties (orbital periods,eccentricities, companion masses, spin periods) and several models have beenput forward that suggest a common formation channel. In this work we presentthe results of an extensive timing campaign focusing on one member of this newpopulation, PSR J1946+3417. Through measurement of the both the advance ofperiastron and Shapiro delay for this system, we determine the mass of thepulsar, companion and the inclination of the orbit to be 1.828(22) Msun,0.2656(19) Msun and 76.4(6) , under the assumption that general relativity isthe true description of gravity. Notably, this is the third highest massmeasured for any pulsar. Using these masses and the astrometric properties ofPSR J1946+3417 we examine three proposed formation channels for eccentric MSPbinaries. While our results are consistent with eccentricity growth driven by acircumbinary disk or neutron star to strange star phase transition, we rule outrotationally delayed accretion-induced collapse as the mechanism responsiblefor the configuration of the PSR J1946+3417 system.

A Massive Millisecond Pulsar in an Eccentric Binary