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Table 1

Spin properties of Galactic BNS pulsars: the period (P), derivative of the period (), frequency (v), derivative of the frequency (v˙$\dot v$), and the references (Ref.) for the listed values.

BNS pulsar P v v˙$\dot v$ Ref.
(10−3 s) (10−18 ss−1) (10−15s−2)
J0737−3039A(a) (…) (…) 44.05406864196281(17) −3.4158071(11) 1
J0737−3039B(a) (…) (… ) 0.36056035506(1) −0.116(1) 2
B1913+16 (…) (… ) 16.940537785677(3) −2.4733(1) 3
J1913+1102 24.2850068680286(19) 0.15672(7) (… ) (… ) 4
J0509+3801 76.5413487220(1) 7.931(2) (… ) (… ) 5
J1756−2251 (… ) (… ) 35.1350727145469(6) −1.256079(3) 6
B1534+12 (… ) (… ) 26.38213277689397(11) −1.686097(2) 7
J1829+2456 (… ) (… ) 24.384401411040(6) −0.029395(14) 8
J1411+2551 62.452895517590(2) 0.0956(51) (… ) (… ) 9
J0453+1559 45.7818168729515(33) 0.18612(8) (… ) (… ) 10
J1518+4904 (… ) (… ) 24.4289793809236(3) −0.0162263(12) 11
J1930−1852 185.52016047926(8) 18.001(6) (… ) (… ) 12

Notes. We follow the literature in giving either P and or v and v˙$\dot v$ for each pulsar, even though these are essentially the same quantities. The values in parentheses show the 1σ uncertainty in the preceding digits. (a)Two components of the double-pulsar binary J0737−3039A/B. (1) Kramer et al. (2021); (2) Kramer et al. (2006); (3) Weisberg & Huang (2016); (4) Ferdman et al. (2020); (5) Lynch et al. (2018); (6) Ferdman et al. (2014); (7) Fonseca et al. (2014); (8) Haniewicz et al. (2021); (9) Martinez et al. (2017); (10) Martinez et al. (2015); (11) Janssen et al. (2008); (12) Swiggum et al. (2015).

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