Collection of some known BeXRPs (shown in black), as well as the accreting millisecond pulsar SAX J1808.4−3658, the intermediate pulsar GRO J1744−28, and the accreting magnetar M82 X-2 (all three shown in blue) on the B−P plane. The solid and dashed lines correspond to the prediction of P^∗(B) from Eq. (13) for β = 1 and two different values of parameter k: 0.5 and 0.7, respectively. This line separates sources where the propeller regime is possible from sources with stable accretion from the cold disc. Persistent low-luminous BeXRPs are shown in green. GRO J1008−57 is shown in red and resides in the area corresponding to the sources with accretion from the cold disc.