Table 1.
Properties of the pulsars considered in the present paper.
| Pulsar | P [ms] | log B [G] | log τ [yr] | d [pc] | Ts∞/(105 K) |
|---|---|---|---|---|---|
| J0437−4715 | 5.75 | 8.45 | 9.82 | 156.96 ± 0.11 |  |
| J2124−3358 | 4.93 | 8.28 | 10.02 |  |
< 4.9 |
| B0950+08 | 253 | 11.38 | 7.24 | 262 ± 5 | 0.6 − 1.2 |
| J0108−1431 | 808 | 11.36 | 8.29 |  |
< 0.6 |
| J2144−3933 | 8510 | 12.27 | 8.43 |  |
< 0.3 |
Notes. The columns contain the name of the pulsar, its rotation period (P), magnetic field strength (B) inferred from spin-down, characteristic age (τ), distance (d), and inferred redshifted surface temperature (Ts∞). The values of P, B, and τ were taken from the ATNF Pulsar Catalogue (https://www.atnf.csiro.au/research/pulsar/psrcat/; Manchester et al. 2005), with B and τ corrected for the “Shklovskii effect” (Shklovskii 1970; Camilo et al. 1994). The (parallax) distance measurements are due to Reardon et al. (2024) (J0437), Reardon et al. (2016) (J2124), Brisken et al. (2002) (B0950), and Deller et al. (2009) (J0108 and J2144). The values of Ts∞ were taken from the HST imaging observations of J2124 (Rangelov et al. 2017), B0950 (Abramkin et al. 2022), J0108 (Abramkin et al. 2021), and J2144 (Guillot et al. 2019), applying recalibrations for J2124 and J2144, and from a joint analysis of spectroscopic HST and ROSAT observations for J0437 (see Sect. 2 and González-Caniulef et al. 2019 for details). The errors are 1σ.
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