I.I. Pronik L.M.Sharipova Crimean Astrophysical Observatory, Nauchny, 98409, Ukrainee

1. Variability of the emission lines in the optical spectrum of the Seyfert galaxy NGC 3227 nucleus in 1966-1992. I.I. Pronik L.M.Sharipova Crimean Astrophysical Observatory, Nauchny, 98409, Ukrainee e-mails:ipronik@crao.crimea.ua, shali@crao.crimea.ua

2. Introduction • NGC 3227 is the bright member of the NGC 3226-3227 pair galaxies. The interaction of these galaxies influenced on the NGC 3227 galaxy activity. • I.I. Pronik revealed the variability of the relative intensity of the emission lines of the galaxy nucleus with time. 1971, Astron.Tsirk.,, N 663, 1.

3. Two day flare by ΔU ~0.5m was recorded by V.M.Lyutyi. 1977, Russ.Astron.J., 54, 1153. • Spectral data in the region 3600-7000ÅÅ allowed I.Pronik to register high maximum of the Hβ brightness in 1975. 1983, Izv. Krimsk. Astrofiz.Obs., 68,81.

4. The UBV observations compiled for 1967-1979 by Quisbert et all. showed essential increase of the nucleus brightness (ΔU ~1m) was in 1975. 1989, PASP, 101, 1078 • Rosenblatt et.all revealed the variability of the Hβ line flux and the continuum flux of the nucleus during 1979-1982. These variations were up to a factor 2 and 3, correspondently. 1992, Astrophys.J.Suppl.Ser., 81,59.

5. I.I. Pronik and L.P. Metik have reviewed the variability of the optical emission lines of the NGC 3227 galaxy nucleus. 2004, Astron. Astrophys. Transact., 23, N 6, 5009. • Investigation of the emission line variability of the NGC 3227 galaxy nucleus in optical spectrum was carried in CrAO about 40 years. It was based on the following data:

6. 1) Spectral data published in literature during 1966-1992. 2) Spectral data obtained during 1971-1981 in CrAO with 2.6-m telescope. 3) Spectral data obtained with 6-m telescope in Special Astrophysical Observatory in January 1977.

7. 1966-1981 • I.I.Pronik used the data obtained with 2.6-m telescope during 1971-1981. The emission lines variability in the optical spectrum of the galaxy nucleus was first revealed on a time scale months, years and high maximum of the Hβ line brightness was registered in 1975. • Changing of the Seyfert type of the galaxy nucleus from Sy2 to Sy1 was first revealed during the epoch of its maximum brightness in 1975 by I.I.Pronik.

8. Three day flare in the emission line region in January 1977 • 53 spectrograms were obtained with 6-m telescope during 4 nights in 1977 by V.L.Afanas’ev. • These data allowed to reveal the three days flare in the region of Balmer emission lines at second and third observational days. Grouping of the profile widths of the Hα, Hβ, Hγ lines was registered. It is shown on Fig.1.

10. Broadening of the hydrogen lines profiles on the 0.5 level of the peak brightness according to Fig.1 was by 12%, 35%, 44% for Hα, Hβ, Hγ lines profiles, correspondently. • Two correlations between ratio Wβ/W[OIII](5007Å) and the width of the Hβ line profile on the 0.5 level of the intensity peak were revealed. They are presented on Fig.2. Left correlation corresponds to 12 and 15 January (first and fourth days of observations). Right correlation corresponds to 13 and 14 January 1977 which were the flare days.

12. 1979-1982 • Rosenblatt et. all investigated the variability of the emission Hβline from March 1979 to May 1982 on the years time scale. Two types of the Hβline profile were revealed . First type is a rectangular shape with a flat core; second type is a triangular shape with distinctly pointed core. Both types are shown on Fig.3 1994, Astrophys.J.Suppl.Ser., 93, 73

14. Rosenblatt et. all assumed that group of the rectangular profiles occur during steady states of the nucleus while the triangular profiles group occur during outbursts. • Using the data of Rosenblatt et. all we obtained two correlations between ratio Wβ/W[OIII](5007Å) and the width of the Hβ line profile on the 0.35 level of its intensity peak. Result is shown on Fig.4.

16. Left and right correlations belong to the triangular and rectangular shape of the Hβ line profile, correspondently. • We suppose that correlations of Fig.4 are similar to correlations obtained for 3 days flare of Fig.2. This lets us to assume: 1) The triangular type of the Hβ line profile exists during the time of the long lived streams of the gas from the galaxy nucleus. 2) The rectangular type of the Hβ line profile appears during the time of a flare.

17. Conclusion • The spectral data of NGC 3227 nucleus obtained during 1971-1981 allowed to register the variability of the relative intensities of the broad and narrow emission lines on the months and years time scales. • Changes of the galaxy Seyfert type nucleus from Sy2 to Sy1 were revealed in 1975. • Three days flare was registered in January 1977. • Two parallel correlations between ratio Wβ/W[OIII](5007Å) and the width of the Hβ line profile were revealed.

18. All spectral data obtained during 1966-1992 allowed to suppose that there is the connection of the spectral line variability of the NGC 3227 galaxy nucleus with three independent emission regions: classical broad line region (BLR), region of long lived streams and region of several days flare. The flare can be connected with shocks in long lived flows from the galaxy nucleus. 2009, I.Pronik, Asron.Astrophys., 496,299.