Black-Hole Transients and the Eddington Limit
  I show that the Eddington limit implies a critical orbital period P_crit(BH) = 2d beyond which black-hole LMXBs cannot appear as persistent systems. The unusual behaviour of GRO J1655-40 may result from its location close to this critical period. 
A.R. King (Astronomy Group, University of Leicester, UK)