Abstract
Abstract We use the intensive optical spectral monitoring of NGC 4151 obtained during the LAG campaign in January—June 1990, to investigate the profile and intensity variations of Hα and Hβ emission lines. The continuum light curve values were supplemented with photoelectrical photometry (11 dates) obtained at the Crimean observatory of the Sternberg Astronomical Institute by V. M. Lyuty. Cross-correlation analysis shows that the time delay between continuum changes and variability of Hβ and Hα is about 4 ± 2 days. The error in the delay was found by applying cross-correlation analysis to a model series, with the same temporal distribution, power spectrum, and signal-to-noise ratio as the actual data. This value of time delay is much lower than was found in other papers for other epochs. We can note two variabilly components in these changes in the lines: one fast and one slow. The amplitude of the slow component relative to the fast component is higher for Hα then for Hβ. The year 1990 was peculiar for N...
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