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The problem on heating the atmospheres of T Tauri stars by radiation from anaccretion shock has been solved. The structure and radiation spectrum of theemerging so-called hot spot have been calculated in the LTE approximation. Theemission not only in continuum but also in lines has been taken into accountfor the first time when calculating the spot spectrum. Comparison withobservations has shown that the strongest of these lines manifest themselves asnarrow components of helium and metal emission lines, while the weaker onesdecrease significantly the depth of photospheric absorption lines, althoughuntil now, this effect has been thought to be due to the emission continuumalone. The veiling by lines changes the depth of different photospheric linesto a very different degree even within a narrow spectral range. Therefore, thenonmonotonic wavelength dependence of the degree of veiling r found for someCTTS does not suggest a nontrivial spectral energy distribution of the veilingcontinuum. In general, it makes sense to specify the degree of veiling r onlyby providing the set of photospheric lines from which this quantity wasdetermined. We show that taking into account the contribution of lines to theveiling of the photospheric spectrum can cause the existing estimates of theaccretion rate onto T Tauri stars to decrease by several times, with this beingalso true for stars with a comparatively weakly veiled spectrum. Neglecting thecontribution of lines to the veiling can also lead to appreciable errors indetermining the effective temperature, interstellar extinction, radialvelocity, and vsin(i).

Interpretation of the Veiling of the Photospheric Spectrum for T Tauri Stars in Terms of an Accretion Model