Table 8.
Published orbital inclinations and Roche-lobe filling factors for the pulsars in our sample.
| Pulsar | Inclination, i (°) | Roche-lobe filling factor, f | Reference | Note |
|---|---|---|---|---|
| J0023+0923 | 54 ± 14 | 0.3 ± 0.3 | Breton et al. (2013) | f = feff |
| 0.2 ± 0.2 | conversion to fL1 | |||
| 77 ± 13 | 0.72 ± 0.04 | Draghis et al. (2019) | ||
| 42 ± 4 | 0.36 ± 0.18 | Mata Sánchez et al. (2023) | ||
| J0610−2100 |  |
 |
van der Wateren et al. (2022) | |
| J0636+5128 | 24.3 ± 3.5 | 0.75 ± 0.20 | Kaplan et al. (2018) | Values for Mp = 1.4M⊙ |
| 23.3 ± 0.3 | 0.98 ± 0.02 | Draghis et al. (2019) | ||
| 24.0 ± 1.0 | f > 0.95 | Mata Sánchez et al. (2023) | ||
| J1124−3653 | 44.9 ± 0.4 | 0.84 ± 0.03 | Draghis et al. (2019) | |
| J1513−2550 | / | / | / | |
| J1544+4937 |  |
f > 0.96 | Mata Sánchez et al. (2023) | |
| J1555−2908 | i > 75 | 0.98 ± 0.02 | Kennedy et al. (2022) | |
| i > 83 | / | Clark et al. (2023) | γ-ray analysis | |
| J1628−3205 | i > 55 | 1 | Li et al. (2014) | f is fixed and not fitted for |
| i < 82.2 | / | Clark et al. (2023) | γ-ray analysis | |
| J1705−1903 | / | / | / | |
| J1719−1438 | / | / | / | |
| J1731−1847 | / | / | / | |
| J1745+1017 | / | / | / | |
| J1959+2048 | 65 ± 2 | 0.81 ≤ f ≤ 0.87 | Reynolds et al. (2007) | |
| 62.5 ± 1.3 | 0.90 ± 0.01 | Draghis et al. (2019) | ||
| i > 84 | / | Clark et al. (2023) | γ-ray analysis | |
| 85.1 ± 0.4 | / | Du et al. (2023) | Radio analysis | |
| J2051−0827 |  |
0.88 ± 0.02 | Dhillon et al. (2022) | |
| 59.5 ± 0.4 | / | Du et al. (2023) | Radio analysis | |
| J2055+3829 | 46.8 ± 1.6 | / | Du et al. (2023) | Radio analysis |
| J2115+5448 | / | / | / | |
| J2214+3000 | / | / | / | |
| J2234+0944 | / | / | / | |
| J2256−1024 | 68 ± 11 | 0.4 ± 0.2 | Breton et al. (2013) | f = feff |
| 0.3 ± 0.1 | conversion to fL1 |
Notes. Two different definitions exist for the filling factor f in these articles. Most articles in this Table define f as the ratio of the companion radius at the nose to the L1 radius. These filling factors, whose values are underlined in the table, are denoted by fL1 and are those used in the rest of the paper. In certain cases f is defined as the ratio of the volume-averaged stellar radius to the volume-averaged Roche lobe radius. These values of f are denoted by feff. To facilitate comparison we converted feff estimates to fL1 estimates when necessary. See Appendix D for details on the conversion. Pulsars marked with a star are those that display eclipses. While most measurements are based on optical photometry of the companion objects, some of the orbital inclination measurements were obtained from radio or γ-ray observations. No constraints on the Roche-lobe filling factor could be obtained from these methods.
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