以下是拟投稿期刊论文的方法部分请进行润色：The initial sample of this paper containing 671 quasars that have at least two-epoch observations provided by Filiz Ak et al 2014 selected from SDSS-IIIIII The details of the sele

The initial sample of this study consisted of 671 quasars with at least two-epoch observations, as selected by Filiz Ak et al. (2014) from SDSS-I/II/III. The selection criteria for these 671 targets were described in Section 2 of Filiz Ak et al. (2014). In their study, Filiz Ak et al. (2014) identified CIV, SiIV, and AlIII BAL/mini-BALs in the spectra of these quasars and classified the CIV BALs into six groups based on the presence or absence of accompanying SiIV and/or AlIIII BALs/mini-BALs at corresponding velocities. Specifically, "CIV00" represents CIV BALs without accompanying SiIV and AlIIII BALs at corresponding velocities during both epochs; "CIVS0" represents CIV BALs with a SiIV BAL at corresponding velocities in one or both epochs, but no corresponding AlIII BAL; "CIVSA" represents CIV BALs with both accompanying SiIV and AlIIII BALs in either epoch; "CIVs0" represents CIV BALs with a SiIV miniBAL, but no accompanying AlIII BAL/mini-BAL is detected; "CIVsa" represents CIV BALs with both accompanying SiIV and AlIIII mini-BALs; and "CIVSa" represents CIV BALs with a SiIV BAL and an AlIIII miniBAL. In addition, Filiz Ak et al. (2014) defined the corresponding SiIV BALs of CIVS0 as "SiIVS0", the corresponding SiIV and AlIIII BALs of CIVSA as "SiIVSA" and "AlIIISA", respectively. It is worth noting that among these nine groups, CIV00, CIVs0, and CIVS0 belong to HiBALs, while CIVsa, CIVSA, CIVSa, SiIVSA, and AlIIISA belong to loBALs.

To calculate the equivalent width (EW) variation (∆W) of all the detected BAL/mini-BALs, we used the EW values measured by Filiz Ak et al. (2014) and applied Equation (1) from Lu et al. (2018). We then selected BALs/mini-BALs based on the criterion of ∆W > 3σ. The number of BALs included in each of the nine groups from Filiz Ak et al. (2014) and those selected for this study are listed in Table 1.

To obtain more accurate flux density values, we downloaded the quasar spectra containing the selected BALs/mini-BALs from the SDSS data set 14 (DR14; Abolfathi et al. 2018). Instead of using the same spectrum as adopted by Filiz Ak et al. (2014), we fitted a power-law continuum for each spectrum using the procedure described in Lu et al. (2018). Finally, we used the power-law continuum flux at 1350 Å from the two-epoch spectra of the same quasar to calculate the fractional variation of the ionizing continuum, following Equation (4) in Lu et al. (2018). We also calculated the fractional variation of BALs using Equation (2) in Lu et al. (2018).

Figure 1 depicts the fractional variation of BALs against the fractional variation of the continuum for each group, and the corresponding results of the Spearman rank correlation analysis are listed in Table 1