Spectroscopic observations of Nova V443 Scuti 1989

Nova 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 B...

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Bibliographic Details
Published in:The Astronomical journal 1991-05, Vol.101 (5), p.1807-1820
Main Authors: ROSINO, L, BENETTI, S, IIJIMA, T, RAFANELLI, P, DELLA VALLE, M
Format: Article
Language:English
Subjects:
640102 - Astrophysics & Cosmology- Stars & Quasi-Stellar, Radio & X-Ray Sources
ABSORPTION SPECTRA
Astronomy
BALMER LINES
BRIGHTNESS
CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS
Earth, ocean, space
EMISSION SPECTRA
ERUPTIVE VARIABLE STARS
Exact sciences and technology
INTERSTELLAR SPACE
IONIZATION
NOVAE
Novae, dwarf novae, recurrent novae, and other cataclysmic (eruptive) variables
OPTICAL PROPERTIES
PHYSICAL PROPERTIES
SPACE
SPECTRA
SPECTROSCOPY
STARS
Variable and peculiar stars (including novae)
VARIABLE STARS
VARIATIONS
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Summary:Nova 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. (Author)
ISSN:0004-6256
1538-3881
DOI:10.1086/115808