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    PR # 31058                                                                   
     If the mass accretion rate onto a strongly magnetized neutron star de       
     creases by three or four orders of magnitude, the Alfven radius incre       
     ases by a factor of about 100. This may result in the significant cha       
     nge in the configuration of accretion flow. Thus the study of the pul       
     se profile, if pulses exist, and the X-ray energy spectrum of such fa       
     int X-ray pulsars is an excellent opportunity for the understanding o       
     f the mass flow and the X-ray emission.  We propose to observe Be tra       
     nsient pulsars in quiescence. The X-ray luminosity of the sources we        
     propose are known to have gone down to 10^33 erg/sec level.                 
                                                                                 
                                                                                 
                                                                                 
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