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Fig. 1


Positions of the LMXBs from Table 1 on the orbital period – X-ray luminosity diagram. Filled circles denote the positions of peculiar systems: grey circles show the positions of binaries with white dwarf or hydrogen-deficit accretors, and the dashed circle shows the position of 4U1822-37 in which we see only a fraction of the total X-ray luminosity due to its nearly edge-on orientation (a so-called accretion disk corona source). The region, occupied by binary systems with a giant donor is shown by the shaded square. The dashed line shows the slope Lx ∝ P2.5 derived by Iben & Tutukov (1984) for the mass transfer rate in binaries in which angular momentum loss is driven by a magnetic stellar wind from a main-sequence donor. The dotted line shows the boundary of persistency according to the thermal-viscous disk instability for binaries with low-mass main-sequence donors Lx/1037 erg/s from Eq. (32) of Dubus et al. (1999), where we adopted M1 = 1.4   M, M2 = 0.4   M, and Lx = 0.1   c2.

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