Table 1.
All known pulsars in Galactic DNS systems and candidates with their spin parameters, orbital parameters, and component masses ordered by merger times τm, including J1208−5936 (highlighted).
| PSR | P0 | Ṗ | Pb | x | e | Mt | Mc | Mp | τm |
|---|---|---|---|---|---|---|---|---|---|
| (ms) | (s s−1) | (days) | (ls) | (M⊙) | (M⊙) | (M⊙) | (Gyr) | ||
| J1946+2052(1) | 16.960 | 9.20 × 10−19 | 0.078 | 1.154 | 0.064 | 2.50(4) | > 1.18 | < 1.31 | ∼0.0455 (a) |
| J1757−1854(2) | 21.497 | 2.63 × 10−18 | 0.184 | 2.238 | 0.606 | 2.732876(8) | 1.3917(4) | 1.3412(4) | 0.0761 |
| J0737−3039A(3) | 22.699 | 1.76 × 10−18 | 0.102 | 1.415 | 0.088 | 2.587052(9) | 1.248868(13) | 1.338185(14) | 0.0860 |
| J0737−3039B(3) | 2773.5 | 8.92 × 10−16 | 0.102 | 1.516 | 0.088 | 2.587052(9) | 1.338185(14) | 1.248868(13) | 0.0860 |
| B1913+16(4) | 59.030 | 8.62 × 10−18 | 0.323 | 2.342 | 0.617 | 2.828(1) | 1.390(1) | 1.438(1) | 0.301 |
| J1906+0746(5) | 144.07 | 2.03 × 10−14 | 0.166 | 1.42 | 0.085 | 2.6134(3) | 1.322(11) | 1.291(11) | 0.308 |
| J1913+1102(6) | 27.285 | 1.61 × 10−19 | 0.206 | 1.755 | 0.090 | 2.8887(6) | 1.27(3) | 1.62(3) | 0.470 |
| J0509+3801(7) | 76.541 | 7.93 × 10−18 | 0.38 | 2.051 | 0.586 | 2.805(3) | 1.46(8) | 1.34(8) | 0.576 |
| J1756−2251(8) | 28.462 | 1.02 × 10−18 | 0.32 | 2.756 | 0.181 | 2.56999(6) | 1.230(7) | 1.341(7) | 1.66 |
| B1534+12(9) | 37.904 | 2.42 × 10−18 | 0.421 | 3.729 | 0.274 | 2.678463(4) | 1.3455(2) | 1.3330(2) | 2.73 |
| J1208–5936(10) | 28.714 | <4 × 10−20 | 0.632 | 4.257 | 0.348 | 2.586(6)(c) |
 (c) |
 (c) |
7.2(2) |
| J1829+2456(11) | 41.010 | 5.25 × 10−20 | 1.176 | 7.238 | 0.139 | 2.60551(19) | 1.299(4) | 1.306(7) | 55 |
| J1325−6253(12) | 28.969 | 4.80 × 10−20 | 1.816 | 7.574 | 0.064 | 2.57(6) | > 0.98 | < 1.59 | ∼189 (a) |
| J1411+2551(13) | 62.453 | 9.56 × 10−20 | 2.616 | 9.205 | 0.17 | 2.538(22) | > 0.92 | < 1.62 | ∼466 (a) |
| J1759+5036(14) | 176.02 | 2.43 × 10−19 | 2.043 | 6.825 | 0.308 | 2.62(3) | > 0.7006 | < 1.9194 | ∼177 (a) |
| J0453+1559(15) | 45.782 | 1.86 × 10−19 | 4.072 | 14.467 | 0.113 | 2.734(4) | 1.174(4) | 1.559(5) | 1453 |
| J1811−1736(16) | 104.18 | 9.01 × 10−19 | 18.779 | 34.783 | 0.828 | 2.57(10) | > 0.93 | < 1.64 | ∼1800 (a) |
| J1518+4904(17) | 40.935 | 2.72 × 10−20 | 8.634 | 20.044 | 0.249 | 2.7183(7) | 1.31(8) | 1.41(8) | 8844 |
| J1018−1523(18) | 83.152 | 1.09(6)×10−19 | 8.984 | 26.157 | 0.228 | 2.3(3) | > 1.16 | < 1.1(3) | ∼1.4(3)×104(a) |
| J1930−1852(19) | 185.52 | 1.80 × 10−17 | 45.06 | 86.89 | 0.399 | 2.59(4) | > 1.30 | < 1.32 | ∼5.32 × 105(a) |
| J1755−2550(20) | 315.20 | 2.43 × 10−15 | 9.696 | 12.284 | 0.089 | ... | > 0.39 | ... | ... (b) |
| J1753−2240(21) | 95.138 | 9.70 × 10−19 | 13.638 | 18.115 | 0.304 | ... | > 0.4875 | ... | ... (b) |
Notes. The first solid line splits systems merging within the Hubble time from those that do not. The last two entries have no total mass measurements, and therefore their DNS nature is uncertain. Nonetheless, they are promising candidates due to their eccentricity.
Total mass quoted from the direct DDGR fit, component masses quoted from the DDGR χ2 mapping marginal one-dimensional likelihood distributions, shown in Fig. 2 and explained in Sect. 3.
References. (1) Stovall et al. (2018), (2) Cameron et al. (2023), (3) Kramer et al. (2021), (4) Weisberg & Huang (2016), (5) van Leeuwen et al. (2015), (6) Ferdman et al. (2020), (7) Lynch et al. (2018), (8) Ferdman et al. (2014), (9) Fonseca et al. (2014), (10) this work, (11) Haniewicz et al. (2021), (12) Sengar et al. (2022), (13) Martinez et al. (2017), (14) Agazie et al. (2021), (15) Martinez et al. (2015), (16) Corongiu et al. (2007), (17) last published work (Janssen et al. 2008) and Sect. 8.3 of Tauris et al. (2017), (18) Swiggum et al. (2023), (19) Swiggum et al. (2015), (20) Ng et al. (2018), and (21) Keith et al. (2009).
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