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tokens: r in = 0.1, and magnetic dipole moment μ 26 = 0.5. It is seen that the model can produce the values measured in the RMSP and LMXB states, consistently with the observed X-ray luminosities. The in the LMXB state is about six times greater than that in the RMSP state. This changes r in only by a small factor of ∼1.09 due to very weak dependence of r in on . The resultant increase in the spin-down torque is also small (∼27 per cent) in good agreement with the observations. Since the accretion and dipole torques are only a few per cent of the torque produced by the disc–field interaction, the onset of accretion with the transition to the weak-propeller phase does not affect significantly. With μ 26 = 4.7, estimated in our model, the dipole torque is found to be about five and seven times smaller than the observed torques in the RMSP and LMXB states, respectively. We note that for r in scaling with r A in the propeller phase, the magnetic torque would be proportional to , implying changes by a factor of ∼5, not in agreement with the measured torques. Table 1. The model parameters and results for J1023. These results are obtained with η = 0.78, Δ r / r in = 0.1, and magnetic dipole moment μ 26 = 0.5. The L x, model values for the high mode and the low mode correspond to L * and L d , respectively. In the last column, Γ acc and Γ tot are the magnitudes of the accretion (spin-up) and the spin-down torques, respectively. For the RMSP state, the observed L x ∼ 10 32 erg s −1 given in Table 1 is the 0.5–10 keV luminosity estimated by Archibald et al. ( 2010 ). From the spectral fits, Li et al. ( 2014 ) estimated that the 3–79 keV luminosity is 5 × 10 32 erg s −1 . In both observations, the X-ray flux was found to be modulated with the orbital motion, which is likely to be due to an intra-binary shock produced by the interaction of pulsar wind with the matter outflowing from the companion. A shock region close to the inner Lagrangian point that is eclipsed when the companion star is between the Earth and the neutron star could explain the observed modulations (Archibald et al. 2010 ; Bogdanov et al. 2011 ; see also Li et al. 2014 for a different interpretation). From the orbital modulations, it is expected that at least half of the X-rays are produced at the shock region in the RMSP state. These observations do not exclude a continuous emission from the disc with r in close to r co characterized by the conditions around the inner disc in the RMSP state. A large fraction of the total L x is emitted by the intra-binary shock modulated by the orbital motion, while the remaining smaller fraction could be produced by the inner disc. The X-ray luminosity estimated in our model is compatible with (smaller than) the continuous portion of the total X-ray luminosity in the RMSP state. We note that the disc emission spectrum could significantly change in the RMSP state due to strong propeller mechanism which can produce not only mass outflow but also hot matter