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Fig. 12


Spin period versus orbital period for a 1.4   M neutron star accretor with a residual equatorial magnetic field of 108.5 G, assuming all transferred matter is propelled out of the system once Rμ > 21/3Rco (solid, Sect. 3.4.2), or hypothetically keeps being accreted (dashed), or hypothetically is accreted at the neutron star surface all the time (dash-dotted). Observed millisecond pulsar-UCXB parameters are represented by filled circles; XTE J1807–294 at an orbital period of 40.07 min (Markwardt et al. 2003a) and a spin period of 5.25 ms (Markwardt et al. 2003b), XTE J1751–305 at 42.42 min, 2.30 ms (Markwardt et al. 2002), XTE J0929–314 at 43.58 min, 5.40 ms (Galloway et al. 2002), SWIFT J1756.9–2508 at 54.70 min, 5.49 ms (Krimm et al. 2007) and NGC 6440 X-2 at 57.3 min, 4.86 ms (Altamirano et al. 2010). The open circle represents 4U 0614+091, which harbors a 2.41 ms pulsar (Strohmayer et al. 2008) and has a tentative orbital period of 51.3 min (Shahbaz et al. 2008; Hakala et al. 2011).

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