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Gray, S. Heatherly, S. Scoles, T. Hockett, T. Snyder","submitted_at":"2015-03-21T07:58:46Z","abstract_excerpt":"In the summer of 2012, during a Pulsar Search Collaboratory workshop, two high-school students discovered J1930$-$1852, a pulsar in a double neutron star (DNS) system. Most DNS systems are characterized by short orbital periods, rapid spin periods and eccentric orbits. However, J1930$-$1852 has the longest spin period ($P_{\\rm spin}\\sim$185 ms) and orbital period ($P_{\\rm b}\\sim$45 days) yet measured among known, recycled pulsars in DNS systems, implying a shorter than average and/or inefficient recycling period before its companion went supernova. 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Cramer, A. Dittmann, A. Laws, A. Vanderhout, B. Miller, B. N. Barlow, C. McGough, C. Pruett, D. R. Lorimer, D. Yencsik, E. Filik, E. Stone, G. Trevino, J. A. Marlowe, J. Fink, J. K. Swiggum, J. Thorley, K. Wenger, L. Teter, M. A. McLaughlin, M. Carter, M. Doehler, M. Hilzendeger, M. Weaver, R. Andrews, R. Crowley, R. Lynch, R. Nunez, R. Rosen, S. Dydiw, S. Ernst, S. Gray, S. Heatherly, S. Scoles, T. Hockett, T. Snyder","submitted_at":"2015-03-21T07:58:46Z","abstract_excerpt":"In the summer of 2012, during a Pulsar Search Collaboratory workshop, two high-school students discovered J1930$-$1852, a pulsar in a double neutron star (DNS) system. Most DNS systems are characterized by short orbital periods, rapid spin periods and eccentric orbits. 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