Modeling the spectrum of V4334 Sgr (Sakurai's object)

Theoretical spectral energy distributions were computed for a grid of hydro gen-deficient and carbon-rich model atmospheres of T-eff in the range of 50 00 - 6250 K and log g = 1.0 - 0.0 by the technique of opacity sampling, tak ing into account continuous molecular band and atomic line absorption. Thes e energy distributions were compared with the spectrum of V4334 Sgr (Sakura i's object) from April, 1997 in the wavelength interval 300 - 1000 nm. We s how that (1) the shape of the theoretical spectra depends strongly on T-eff , but only very weakly on the hydrogen abundance; (2) the comparison of the observed and computed spectra permits us to estimate T-eff approximate to 5500 K for V4334 Sgr in April, 1997, and its interstellar reddening (plus a possible circumstellar contribution) EB-V approximate to 0.70.