Using the stellar population synthesis, we model the stellar contribution fora sample of 110 double-peaked broad-lines AGNs from the Sloan Digital SkySurvey (SDSS). The stellar velocity dispersions ($\sigma_*$) are obtained for52 double-peaked AGNs with obvious stellar absorption features, ranging from106 to 284 \kms. We also use multi-component profiles to fit \OIII$\lambda\lambda4959,5007$ and H$\beta$ emission lines. Using thewell-established $M_{\rm bh}-\sigma_*$ relation, the black hole masses arecalculated to range from $1.0\times 10^{7}$ to $5.5\times 10^{8}$ $\Msun$, andthe Eddington ratio from about 0.01 to about 1. Comparing with the known$R_{\rm BLR}-L$ relation, we can get the factor $f$, which indicates BLRs'geometry, inclination and kinematics. We find that $f$ far deviates from 0.75,suggesting the non-virial dynamics of broad line regions. The peak separationis mildly correlated with the Eddington ratio and SMBH mass with almost thesame correlation coefficients. It implies that it is difficult to detectobvious double-peak AGNs with higher Eddington ratios. Using the monochromaticluminosity at 5100\AA to trace the bolometric luminosity, we find that theexternal illumination of the accretion disk is needed to produce the observedstrength of H$\alpha$ emission line.
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