Stovall, K., Freire, P. C. C., Chatterjee, S., Demorest, P. B., Lorimer, D. R., McLaughlin, M. A., Pol, N., van Leeuwen, J., Wharton, R. S., Allen, B., Boyce, M., Brazier, A., Caballero, K., Camilo, F., Camuccio, R., Cordes, J. M., Crawford, F., Deneva, J. S., Ferdman, R. D. ORCID: https://orcid.org/0000-0002-2223-1235, Hessels, J. W. T., Jenet, F. A., Kaspi, V. M., Knispel, B., Lazarus, P., Lynch, R., Parent, E., Patel, C., Pleunis, Z., Ransom, S. M., Scholz, P., Seymour, A., Siemens, X., Stairs, I. H., Swiggum, J. and Zhu, W. W. (2018) PALFA discovery of a highly relativistic double neutron star binary. The Astrophysical Journal Letters, 854. ISSN 2041-8205
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Abstract
We report the discovery and initial follow-up of a double neutron star (DNS) system, PSR J1946+2052, with the Arecibo L-Band Feed Array pulsar (PALFA) survey. PSR J1946+2052 is a 17 ms pulsar in a 1.88 hr, eccentric (e = 0.06) orbit with a gsim1.2 M ⊙ companion. We have used the Jansky Very Large Array to localize PSR J1946+2052 to a precision of 0farcs09 using a new phase binning mode. We have searched multiwavelength catalogs for coincident sources but did not find any counterparts. The improved position enabled a measurement of the spin period derivative of the pulsar ($\dot{P}=9\pm 2\times {10}^{-19}$); the small inferred magnetic field strength at the surface (B S = 4 × 109 G) indicates that this pulsar has been recycled. This and the orbital eccentricity lead to the conclusion that PSR J1946+2052 is in a DNS system. Among all known radio pulsars in DNS systems, PSR J1946+2052 has the shortest orbital period and the shortest estimated merger timescale, 46 Myr; at that time it will display the largest spin effects on gravitational-wave waveforms of any such system discovered to date. We have measured the advance of periastron passage for this system, $\dot{\omega }=25.6\pm 0.3\,\deg \,{\mathrm{yr}}^{-1}$, implying a total system mass of only 2.50 ± 0.04 M ⊙, so it is among the lowest-mass DNS systems. This total mass measurement combined with the minimum companion mass constrains the pulsar mass to lesssim1.3 M ⊙.
Item Type: | Article |
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Uncontrolled Keywords: | pulsars,individual (psr j1946+2052) |
Faculty \ School: | Faculty of Science > School of Chemistry (former - to 2024) |
UEA Research Groups: | Faculty of Science > Research Groups > Quantum Matter Faculty of Science > Research Groups > Numerical Simulation, Statistics & Data Science |
Depositing User: | LivePure Connector |
Date Deposited: | 06 Jul 2018 11:30 |
Last Modified: | 07 Nov 2024 12:40 |
URI: | https://ueaeprints.uea.ac.uk/id/eprint/67535 |
DOI: | 10.3847/2041-8213/aaad06 |
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