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PALFA Discovery of a Highly Relativistic Double Neutron Star Binary | | K. Stovall
; P. C. C. Freire
; S. Chatterjee
; P. B. Demorest
; D. R. Lorimer
; M. A. McLaughlin
; N. Pol
; J. van Leeuwen
; R. S. Wharton
; B. Allen
; M. Boyce
; A. Brazier
; K. Caballero
; F. Camilo
; R. Camuccio
; J. M. Cordes
; F. Crawford
; J. S. Deneva
; R. D. Ferdman
; J. W. T. Hessels
; F. A. Jenet
; V. M. Kaspi
; B. Knispel
; P. Lazarus
; R. Lynch
; E. Parent
; C. Patel
; Z. Pleunis
; S. M. Ransom
; P. Scholz
; A. Seymour
; X. Siemens
; I. H. Stairs
; J. Swiggum
; W. W. Zhu
; | | Date: |
5 Feb 2018 | | Abstract: | We report the discovery and initial follow-up of a double neutron star (DNS)
system, PSR J1946$+$2052, with the Arecibo L-Band Feed Array pulsar (PALFA)
survey. PSR J1946$+$2052 is a 17-ms pulsar in a 1.88-hour, eccentric ($e , =,
0.06$) orbit with a $gtrsim 1.2 , M_odot$ companion. We have used the Jansky
Very Large Array to localize PSR J1946$+$2052 to a precision of 0.09 arcseconds
using a new phase binning mode. We have searched multiwavelength catalogs for
coincident sources but did not find any counterparts. The improved position
enabled a measurement of the spin period derivative of the pulsar ($dot{P} ,
= , 9,pm , 2 , imes 10^{-19}$); the small inferred magnetic field
strength at the surface ($B_S , = , 4 , imes , 10^9 ,
m 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, $dot{omega} , = , 25.6 , pm , 0.3, deg
m yr^{-1}$, implying
a total system mass of only 2.50 $pm$ 0.04 $M_odot$, so it is among the
lowest mass DNS systems. This total mass measurement combined with the minimum
companion mass constrains the pulsar mass to $lesssim 1.3 , M_odot$. | | Source: | arXiv, 1802.1707 | | Services: | Forum | Review | PDF | Favorites | |
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