We study observed optical-ultraviolet spectral energy distribution of 10 weak emission-line quasars ( WLQs ) which lie at redshifts z = 0.19 and 1.43 < z < 3.48 .
The theoretical models of their accretion disc continua are created based on the Novikov-Thorne equations .
It allows us to estimate masses of their supermassive black holes ( M _ { \mathrm { BH } } ) and accretion rates .
We determine the virial factor for WLQs and note its anti-correlation with the full width at half maximum ( FWHM ) of H \beta emission-line ( f \propto \mathit { FWHM } ^ { \alpha } , \alpha = -1.99 \pm 0.67 ) .
By comparison with the estimated previously BH masses , the underestimation of M _ { \mathrm { BH } } is noticed with a mean factor 7.4 dependent on the measured full width .
We propose the new formula to estimate M _ { \mathrm { BH } } in WLQs based on their observed FWHM ( H \beta ) and luminosities at 5100Å .
In our opinion , WLQs are also normal quasars visible in a reactivation stage .