Evidence for “propeller” Effects in X-ray Pulsars Gx 114 and Gro J1744228

We present observational evidence for “propeller” effects in two X-ray pulsars, GX 114 and GRO J1744228. Both sources were monitored regularly by the Rossi X-ray Timing Explorer (RXTE) throughout a decay period in the X-ray brightness. Quite remarkably, strong X-ray pulsation became unmeasurable when total X-ray flux had dropped below a certain threshold. Such a phenomenon is a clear indication of the propeller effects that take place when pulsar magnetosphere grows beyond the co-rotation radius as a result of the decrease in mass accretion rate and the centrifugal force prevents accreting matter from reaching the magnetic poles. The entire process should simply reverse as the accretion rate increases. Indeed, steady X-ray pulsation was reestablished as the sources emerged from the nonpulsating faint state. These data allow us to directly derive the surface polar magnetic field strength for both pulsars: 3.1 3 10 G for GX 114 and 2.4 3 10 G for GRO J1744228. The results are likely to be accurate to within a factor of 2, with the total uncertainty dominated by the uncertainty in estimating the distances to the sources. Possible mechanisms for the persistent emission observed in the faint state are discussed in light of the extreme magnetic properties of the sources. Subject headings: accretion, accretion disks— stars: pulsars: individual (GX 114, GRO J1744228)— X-rays: stars