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We studied optical-ultraviolet spectral energy distribution of 10 weak emission-line quasars (WLQs) that lie at redshifts z = 0.19 and 1.43 < z < 3.48. The theoretical models of their accretion disk continua are created based on the Novikov–Thorne equations. It allows us to estimate masses of their supermassive black holes () and accretion rates. We determined the virial factor for WLQs and note its anticorrelation with the FWHM of the Hβ emission line). By comparison with the previously estimated BH masses, the underestimation of is noticed with a mean factor of 4–5, which depends on the measured full width. We proposed a new formula to estimate in WLQs based on their observed (Hβ) and luminosities at 5100 Å. In our opinion, WLQs are also normal quasars visible in a reactivation stage. [ABSTRACT FROM AUTHOR]