Evolution of selected binaries from our simulated grids for β = 0.3, f_pular = 0.0, and $M_{\mathrm{NS}}^i=1.3{\mathrm{M}}_{\odot }$. The three different kinds of binaries that we discuss in the text are studied here: case A ($P_{\mathrm{orb}}^i=1.0$ d), near-P_bif ($P_{\mathrm{orb}}^i=2.4$ d), and case B or diverging ($P_{\mathrm{orb}}^i=2.6$ d). Also shown is the binary that goes down to the orbital period of 19 min (orange curve) for comparison, which is the minimum in the grid with f_pulsar = 0.0. Top left shows the orbital period versus companion mass, where M_c is the mass of the companion to the NS and P_orb is the orbital period. The formation of a fully convective star and the start of the ejection phase are shown as squares. We also compare our tracks to estimated M_c, min and observed 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 tidarrens, namely, J1311–3430, J1653–0159, and J0636+5128, are highlighted as pink, blue, and black crosses, respectively. Top right, bottom left, and bottom right show the time evolution of the NS spin, companion mass loss rate, and NS mass, respectively, for the same binaries. The time axis is zoomed in to focus on the spin-up phase.