Rosino, L.L.RosinoBENETTI, StefanoStefanoBENETTIIijima, T.T.IijimaRafanelli, P.P.RafanelliDELLA VALLE, MassimoMassimoDELLA VALLE2022-09-282022-09-2819910004-6256http://hdl.handle.net/20.500.12386/32663Nova V443 Scuti 1989 reached its maximum, of visual magnitude about 7.5, very likely on September 13-14, 1989, displaying in its early decline brightness fluctuations of relatively large amplitude with a periodicity of about 17 days. In October the spectrum was characterized by the presence of the Balmer emission lines and by those of Fe II, Na I, Ti II, O I, N II accompanied by two systems of displaced P Cyg absorptions, having an average velocity of about -710 and -1460 km/s. The transition phase took place in November, with the appearance of forbidden N II 5755 and O II 7319 -30 and with the O I 6300 - 6364 flash. In March 1990, the nova was found in the nebular phase with wide emission lines of H, He I, He II, and collisionally excited lines of forbidden N II, O II, O III, and Ne III. From April to July, the degree of ionization having further progressed, forbidden lines of Fe VI, Fe VII, A III, A IV, A V, Ca V, and possibly also of Fe X, emerged.STAMPAenArticle10.1086/1158082-s2.0-12044259067https://ui.adsabs.harvard.edu/abs/1991AJ....101.1807R/abstracthttps://api.elsevier.com/content/abstract/scopus_id/120442590671991AJ....101.1807RFIS/05 - ASTRONOMIA E ASTROFISICA