  We study the giant outbursts of SMC X-3 and RX J0209.6-7427 to compare their
super-Eddington accretion regime with that of Swift J0243.6+6124. The high
double-peak profile of SMC X-3 is found to be 0.25 phase offset from that below
$2.3\times10^{38}$erg\,s$^{-1}$, which is similar to Swift J0243 (happened
around $0.9\times10^{38}$erg\,s$^{-1}$). The profile of RX J0209 shows a
similar 0.25 phase offset between high double-peak and low double-peak around
$1.25\times10^{38}$erg\,s$^{-1}$. The 0.25 phase offset corresponds to a 90
degree angle change of the emission beam and strongly supports for a transition
from a fan beam to a pencil beam. Their critical luminosities imply a surface
magnetic field $\sim4\times10^{13}$ G and $2\times10^{13}$ G for SMC X-3 and RX
J0209, respectively, based on the recently measured cyclotron line of Swift
J0243. The spin-up rate and luminosity of SMC X-3 follows a relation of
$\dot{\nu}\propto L^{0.94\pm0.03}$, while that of RX J0209 follows
$\dot{\nu}\propto L^{1.00\pm0.03}$, which are similar to Swift J0243 and
consistent with the prediction of a radiation-pressure-dominated (RPD) disk.
These results indicate that accretion columns are indeed formed above Eddington
luminosity, and the population of ULXPs likely corresponds to X-ray pulsars of
highest magnetic field.
