SIMBAD references

2015ApJ...805..156S - Astrophys. J., 805, 156 (2015/June-1)

PSR J1930-1852: a pulsar in the widest known orbit around another neutron star.

SWIGGUM J.K., ROSEN R., McLAUGHLIN M.A., LORIMER D.R., HEATHERLY S., LYNCH R., SCOLES S., HOCKETT T., FILIK E., MARLOWE J.A., BARLOW B.N., WEAVER M., HILZENDEGER M., ERNST S., CROWLEY R., STONE E., MILLER B., NUNEZ R., TREVINO G., DOEHLER M., CRAMER A., YENCSIK D., THORLEY J., ANDREWS R., LAWS A., WENGER K., TETER L., SNYDER T., DITTMANN A., GRAY S., CARTER M., McGOUGH C., DYDIW S., PRUETT C., FINK J. and VANDERHOUT A.

Abstract (from CDS):

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 (Pspin ∼ 185 ms) and orbital period (Pb ∼ 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. We measure the relativistic advance of periastron for J1930-1852, ω = 0.00078 (4) deg/yr, which implies a total mass (Mtot = 2.59 (4) M☉) consistent with other DNS systems. The 2σ constraints on Mtot place limits on the pulsar and companion masses (mp < 1.32M☉ and mc > 1.30 M☉ respectively). J1930-1852's spin and orbital parameters challenge current DNS population models and make J1930-1852 an important system for further investigation.

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Journal keyword(s): pulsars: general - pulsars: individual: J1930-1852 - stars: evolution - stars: neutron

Simbad objects: 14

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