Modeling the spectrum of V 4334 Sgr ( Sakurai ’ s object ) Ya

Theoretical spectral energy distributions were computed for a grid of hydrogen-deficient and carbon-rich model atmospheres of Teff in the range of 5000− 6250 K and log g = 1.0− 0.0 by the technique of opacity sampling, taking into account continuous molecular band and atomic line absorption. These energy distributions were compared with the spectrum of V4334 Sgr (Sakurai’s object) from April, 1997 in the wavelength interval 300 − 1000 nm. We show that (1) the shape of the theoretical spectra depends strongly on Teff , but only very weakly on the hydrogen abundance; (2) the comparison of the observed and computed spectra permits us to estimate Teff ≈ 5500 K for V4334 Sgr in April, 1997, and its interstellar reddening (plus a possible circumstellar contribution) EB−V ≈ 0.70.