Orbital period evolution versus companion mass of selected binaries from our simulated grid shown in Figure 1. The term M_c is the mass of the companion to the NS, and P_orb is the orbital period. The figure shows the effect of pulsar wind irradiation, comparing f_pulsar = 0.0 (dashed lines) and 0.5 (solid lines). The left panel shows the tracks with $M_{\mathrm{c}}^i=1.5{\mathrm{M}}_{\odot }$, $P_{\mathrm{orb}}^i=1.0$, 2.4, and 2.6 d. The right panel shows two initial companion masses, $M_{\mathrm{c}}^i=1.0$ (with $P_{\mathrm{orb}}^i=1$ d) and 2.5 M_⊙ ($P_{\mathrm{orb}}^i=2.0$ and 2.2 d). We compared our tracks to M_c, min and P_orb for BWs (faint black crosses), RBs (faint red crosses), and huntsmen spiders (faint green crosses), from Nedreaas (2024, and references therein). The green star is the huntsman candidate 2FGL J0846.0+2820, observed by Fermi-LAT (Swihart et al. 2017). The magenta stars show the three transitional MSPs (tMSPs) observed, PSR J1023+0038 (M_c = 0.22 M_⊙ and P_orb = 4.75 h; Shahbaz et al. 2019; Thorstensen & Armstrong 2005), IGR J18245–2452 (M_c, min = 0.17 M_⊙ and P_orb = 11.03 h; Papitto et al. 2013), and XSS J12270–4859 (M_c, min = 0.15 M_⊙ and P_orb = 6.91 h; Roy et al. 2015; de Martino et al. 2015; Bassa et al. 2014).