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Fig. 9


Correlation between a combination of the propeller limiting luminosity and the pulsar spin period, LlimP7 / 3, and independently determined magnetic field strength B for six pulsating sources (black squares; adopted from Tsygankov et al. 2016a). The dashed line represents the theoretical dependence given by Eq. (2) for k = 0.5. Estimate of the limiting luminosity and corresponding dipole field strength for SMC X-3 are shown with horizontal shaded region and dotted vertical lines, respectively. The solid red vertical line indicates the dipole field estimate from the observed spin evolution of the source. Constraints on the field strength in vicinity of the NS based on the observed critical and maximal luminosities are shown with vertical shaded region. We note an order of magnitude discrepancy between the field estimates at the magnetosphere and in vicinity of the NS. Green circles show similar discrepancy between two field components in the pulsating ULXs in NGC 5907 and NGC 7793 P13.

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