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The spectral energy distribution (SED) of the TT Ari system, which is wellknown from published IUE and optical photometric observations, was modeled by asteady-state accretion \alpha-disc around a white dwarf. Parameters of thesystem were derived from time-resolved optical spectral observations in thebright state that we obtained in Sep. 1998. The radial velocity semi-amplitudeof the white dwarf (33.8 +/- 2.5 km/s) and corresponding mass function (f(M) =5.5 +/- 1.2 *10^{-4}~ M_sun) were derived from the motion of the emissioncomponents of Balmer lines. The mass ratio q (\approx 0.315) was evaluated fromthe fractional period excess of the superhump period over the orbital period\epsilon (\approx 0.085), and a secondary mass range (0.18 - 0.38 M_sun) wasestimated from the orbital period. Therefore, the white dwarf mass range is0.57 - 1.2 M_sun and the inclination angle of the system to the line of sightis 17 - 22.5 degrees. The adopted distance to the system is 335 +/- 50 pc. Tofit the observed SED it is necessary to add a thermal spectrum with T \approx11600 K and luminosity \approx 0.4 L_disk to the accretion disc spectrum. Thiscombined spectrum successfully describes the observed Balmer lines absorptioncomponents. Formally the best fit of the HeI 4471 line gives minimum masses ofthe components (M_RD = 0.18 M_sun and M_WD = 0.57 M_sun), with thecorresponding inclination angle i = 22.1 deg and mass-accretion rate \dot M =2.6 * 10^{17} g/s.

Modeling of the spectral energy distribution of the cataclysmic variable TT Ari and evaluation of the system parameters