@article {41769,
	title = {Comparing the super-Eddington accretion of SMC X-3 and RX J0209.6-7427 with Swift J0243.6+6124},
	volume = {517},
	year = {2022},
	month = {2022/12/1},
	pages = {3354 - 3361},
	publisher = {OUP},
	abstract = {We study the giant outbursts of SMC X-3 and RX J0209.6-7427 (hereafter RX J0209) to compare their super-Eddington accretion regime with that of Swift J0243.6+6124 (hereafter Swift J0243). The high double-peak profile of SMC X-3 is found to be 0.25 phase offset from that below 2.3 {\texttimes} 10<SUP>38</SUP> erg s<SUP>-1</SUP>, which is similar to Swift J0243 (happened around 0.9 {\texttimes} 10<SUP>38</SUP> erg s<SUP>-1</SUP>). The profile of RX J0209 shows a similar 0.25 phase offset between high double-peak and low double-peak around 1.25 {\texttimes} 10<SUP>38</SUP> erg s<SUP>-1</SUP>. The 0.25 phase offset corresponds to a 90{\textdegree} 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 ~4 {\texttimes} 10<SUP>13</SUP> and 2 {\texttimes} 10<SUP>13</SUP> 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 $\dot{\nu }\propto L^{0.94\pm 0.03}$, while that of RX J0209 follows $\dot{\nu }\propto L^{1.00\pm 0.03}$, which are similar to Swift J0243 and consistent with the prediction of a radiation-pressure-dominated disc. These results indicate that accretion columns are indeed formed above Eddington luminosity, and the population of ultraluminous X-ray pulsars likely corresponds to X-ray pulsars of highest magnetic field.},
	keywords = {Accretion, accretion discs, Astrophysics - High Energy Astrophysical Phenomena, pulsars: individual: RX J0209.6-7427, pulsars: individual: SMC X-3, pulsars: individual: Swift J0243.6+6124, X-rays: binaries},
	isbn = {0035-8711},
	url = {https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.3354L},
	author = {Liu, Jiren and Vasilopoulos, Georgios and Ge, MingYu and Ji, Long and Weng, Shan-Shan and Zhang, Shuang-Nan and Hou, Xian}
}
