论文标题
第一个银河超光的X射线脉冲星Swift J0243.6+6124的超级埃德丁顿积聚
Super-Eddington accretion of the first Galactic Ultra-luminous X-ray pulsar Swift J0243.6+6124
论文作者
论文摘要
我们在其2017年巨人爆发期间，介绍了Swift J0243.6+6124的脉冲研究的详细计时研究。亮度高于$ 5 \ times10^{38} $ erg \ \，s $^{ - 1} $的双峰式配置文件与低于$ 1.5 \ times10^{38} $ erg \ erg \ erg \ erg \，s $^{ - 1} $的相距为0.25阶段，从而从粉丝启用了polen beam to polen the in the ockret and ockret to poldion to poldion to polen to polen the the Meakition，并启用了polle polen的形式。在高双峰政权的上升阶段，微弱的峰在$ l_t \ sim1.3 \ sim1.3 \ times10^{39} $ erg \，s $^{ - 1} $上方的10-100 keV频段中饱和，这与主要和微弱的峰的突然变化是一致的。这意味着在$ l_t $上突然改变排放模式。旋转率（$ \dotν$）与低于$ l_t $的发光度（$ l $）线性相关，这与预测辐射压力（RPD）磁盘的预测一致。 $ \dotν-l $关系在$ l_t $上面变平，这表明角动量的效率较低，并且在$ l_t $上方的积聚磁盘几何形状的变化。这很可能是由于中央积聚柱对磁盘的辐照，并在内部磁盘半径达到球形半径之前表明明显的辐射反馈。
We present a detailed timing study of the pulse profile of Swift J0243.6+6124 with HXMT and Fermi/GBM data during its 2017 giant outburst. The double-peak profile at luminosity above $5\times10^{38}$erg\,s$^{-1}$ is found to be 0.25 phase offset from that below $1.5\times10^{38}$erg\,s$^{-1}$, which strongly supports for a transition from a pencil beam to a fan beam, and thus for the formation of shock dominated accretion column. During the rising stage of the high double-peak regime, the faint peak got saturated in 10-100 keV band above a luminosity of $L_t\sim1.3\times10^{39}$erg\,s$^{-1}$, which is coincident with sudden spectral changes of both the main and faint peaks. They imply a sudden change of emission pattern around $L_t$. The spin-up rate ($\dotν$) is linearly correlated with luminosity ($L$) below $L_t$, consistent with the prediction of a radiation pressure dominated (RPD) disk. The $\dotν-L$ relation flattens above $L_t$, indicating a less efficient transfer of angular momentum and a change of accretion disk geometry above $L_t$. It is likely due to irradiation of the disk by the central accretion column and indicates significant radiation feedback before the inner disk radius reaching the spherization radius.
