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tokens: panel), 95701-01-03-00 ( km, middle panel), and 91701-01-52-01 ( km, bottom panel), respectively. 3.2. Spectral Parameters The spectral fitting results are presented in Figure 5 . The unabsorbed power-law luminosity ( L PL ) and the disk luminosity increase simultaneously with the total luminosity ( L 3–30 keV ). The apparent inner disk radius ( R in ) is related to the disk normalization as , where D 10 is the distance in units of 10 kpc. Here we adopt the inclination angle θ = 66° (Fender et al. 1999 ), a color correction factor f = 1.9 (Neilsen et al. 2011 ), and a distance of 8.6 kpc (Reid et al. 2014 ) in the calculation. There are two branches shown in the diagrams of L 3–30 keV − R in and L 3–30 keV − kT : (1) The inner disk remains at a small radius ( R in ≤ 70 km, hereafter S branch), kT increases with the X-ray luminosity, and the X-ray emissions are fainter and softer (larger Γ). (2) The majority of data (189 out of 233) draw the other branch (L branch), the apparent inner edge of disk recedes, and the temperature increases slowly at high luminosity. Meanwhile, the photon index (Γ) of the nonthermal component is anticorrelated with the X-ray luminosity. Figure 5. Correlations between the spectral parameters and distribution of the reduced χ 2 with the fitting model of diskbb + powerlaw (right bottom panel). Open squares and filled cycles correspond to the data with R in being smaller and larger than 70 km, respectively. All parameters are plotted with their 1 σ errors. Intriguingly, there are the positive correlations between T rec , R in , and the X-ray luminosity as well. Additionally, T rec has an even tighter correlation with the power-law luminosity. Since the uncertainty on T rec is much larger than on L 3–30 keV , we carry out a power-law fit to the relation by taking the error on T rec into account, yielding an index of n = 1.10 ± 0.10. Meanwhile, T rec is proportional to . It is worth noting that the change of apparent inner disk radius can be interpreted as a varying color correction factor without moving the intrinsic inner disk radius (e.g., Merloni et al. 2000 ; Zoghbi et al. 2016 ). In order to check this scenario, we model the disk component with diskpn (Gierliński et al. 1999 ), in which the disk normalization is linked to the color correction factor: . The inner disk radius is fixed to the bottom limit 6 R g , although it is much smaller due to high spinning rate (McClintock et al. 2006 ). In addition, the power-law model is replaced by a physical Comptonization model ( tbabs*(diskpn + comptt) in XSPEC). We tie the seed temperature ( kT seed ) to the disk temperature and fix the plasma temperature to 50 keV because it cannot be constrained by our data. The data in the S branch are relatively soft, and the model described above cannot provide an adequate fit to them unless the kT seed varies freely and becomes hotter than the disk temperature; however, it is inconsistent. Henceforth, we only fit the data in the L