Using the stellar population synthesis , we model the stellar contribution for a sample of 110 double-peaked broad-lines AGNs from the Sloan Digital Sky Survey ( SDSS ) . The stellar velocity dispersions ( \sigma _ { * } ) are obtained for 52 double-peaked AGNs with obvious stellar absorption features , ranging from 106 to 284 km s ^ { -1 } . We also use multi-component profiles to fit [ O~ { } \sc { III } ] \lambda \lambda 4959 , 5007 and H \beta emission lines . Using the well-established M _ { bh } - \sigma _ { * } relation , the black hole masses are calculated to range from 1.0 \times 10 ^ { 7 } to 5.5 \times 10 ^ { 8 } M _ { \odot } , and the Eddington ratio from about 0.01 to about 1 . Comparing with the known R _ { 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 separation is mildly correlated with the Eddington ratio and SMBH mass with almost the same correlation coefficients . It implies that it is difficult to detect obvious double-peak AGNs with higher Eddington ratios . Using the monochromatic luminosity at 5100Å to trace the bolometric luminosity , we find that the external illumination of the accretion disk is needed to produce the observed strength of H \alpha emission line .