| DOI | Resolve DOI: https://doi.org/10.3847/2041-8213/aaad06 |
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| Author | Search for: Stovall, K.; Search for: Freire, P. C. C.; Search for: Chatterjee, S.; Search for: Demorest, P. B.; Search for: Lorimer, D. R.; Search for: Mclaughlin, M. A.; Search for: Pol, N.; Search for: Van Leeuwen, J.; Search for: Wharton, R. S.; Search for: Allen, B.; Search for: Boyce, M.; Search for: Brazier, A.; Search for: Caballero, K.; Search for: Camilo, F.; Search for: Camuccio, R.; Search for: Cordes, J. M.; Search for: Crawford, F.; Search for: Deneva, J. S.; Search for: Ferdman, R. D.; Search for: Hessels, J. W. T.; Search for: Jenet, F. A.; Search for: Kaspi, V. M.1; Search for: Knispel, B.; Search for: Lazarus, P.; Search for: Lynch, R.; Search for: Parent, E.; Search for: Patel, C.1; Search for: Pleunis, Z.1; Search for: Ransom, S. M.; Search for: Scholz, P.; Search for: Seymour, A.; Search for: Siemens, X.; Search for: Stairs, I. H.1; Search for: Swiggum, J.; Search for: Zhu, W. W. |
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| Affiliation | - National Research Council of Canada. Herzberg Astronomy and Astrophysics
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| Format | Text, Article |
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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 (P=9 +- 2 x10 ^(-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, omega = 25.6 +- 0.3 deg 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 ⊙. |
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| Publication date | 2018-02-16 |
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| Publisher | American Astronomical Society |
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| In | |
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| Language | English |
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| Peer reviewed | Yes |
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| NPARC number | 23003822 |
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| Export citation | Export as RIS |
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| Report a correction | Report a correction (opens in a new tab) |
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| Record identifier | 0d418543-b7a9-4a78-bff1-9d73820606cb |
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| Record created | 2018-08-13 |
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| Record modified | 2020-03-16 |
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