$\sim1.5\cdot10^{33}$ erg/s while the nonzero moderate flux was measured [@Muk05]. This means at such luminosity a transition between centrifugal inhibition and direct accretion when a fraction of the disk material is going onto the surface of the NS along the magnetic field lines. The luminosity obtained in the BeppoSax-NFI observations gives for A0535+262 in quiescence an accretion rate $\dot{M} = 2.05\cdot10^{13}$ g/s and magnetospheric radius $r_m$ about $9.35\cdot10^9$ cm [@Muk05].

In the case of type 1 outbursts caused by the wind-fed accretion, there will be less efficient angular momentum transfer compared to a standard transfer disk accretion [@Ina04]. On the contrary, the disk-fed accretion can transfer angular momentum either at the vicinity of the magnetosphere radius where the disc is disrupted and the material is channeled from the inner edge of the disc to the magnetic poles, or from the overall interaction of the accretion disc and magnetic field lines of the NS. Thus, the material torque from a prograde accretion disk, being proportional to mass accretion rate, always acts to spin-up the NS, while the contribution of magnetic torque from the magnetic field lines threading the disk outside the corotation radius is negative. The resultant torque can either be 