Table 1
Neutron stars that are candidates for being formed via AIC in a globular cluster (a–d) or in the Galactic disk (e–h), respectively.
| Object | P | B* | Porb |
|
Ref. |
| ms | G | days | M⊙ | ||
|
|
|||||
| PSR B1718−19 | 1004 | 4.0 × 1011 | 0.258 | ~0.10 | a |
| PSR J1745−20A | 289 | 1.1 × 1011 | – | – | b |
| PSR J1820−30B | 379 | 3.4 × 1010 | – | – | c |
| PSR J1823−3021C | 406 | 9.5 × 1010 | – | – | d |
|
|
|||||
| GRO J1744−28 | 467 | 1.0 × 1013 | 11.8 | ~0.08 | e |
| PSR J1744−3922 | 172 | 5.0 × 109 | 0.191 | ~0.10 | f |
| PSR B1831−00 | 521 | 2.0 × 1010 | 1.81 | ~0.08 | g |
| 4U 1626−67 | 7680 | 3.0 × 1012 | 0.028 | ~0.02 | h |
Notes.See text for explanations and discussion.
B-field values calculated from Eq. (5) in Tauris et al. (2012) which includes a spin-down torque due to a plasma-filled magnetosphere.
Reference. a) Lyne et al. (1993); b) Lyne et al. (1996); c) Biggs et al. (1994); d) Boyles et al. (2011); e) van Paradijs et al. (1997); f) Breton et al. (2007); g) Sutantyo & Li (2000); h) Yungelson et al. (2002).
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