Visible and/or near infrared spectral variations of v1016 Cygni,HM sagittae and MWC 349

The recent spectral evolution of the three peculiar emission-line objects with IR excess V1016 Cyg, HM Sge, and MWC 349 is described, on the basis of data obtained at the Asiago (blue and red spectral regions) and Haute Provence (near infrared) Observatories. In the near infrared spectral region, details are given concerning the data briefly described in IAU Circular No. 3498 (Andrillat and Swings, 1980).Based on observations performed at the Haute Provence (CNRS, France) and Asiago (Italy) Observatories.     

The spectrum of nova vulpeculae 1984 No2 at nebular phase

Nova Vul 1984 n^o2 has been again observed at Observatoire de Haute-Provence in the autumn of 1985, i.e. 270–295 days after maximum. It was then in the nebular phase. The spectra cover the blue-violet and the near infrared regions. Over 50 lines and blends have been identified and are given in Table 2. No clear pattern is observed in the emission bands of a width of about 1450 km/sec. The most conspicuous features observed are the forbidden NeIII and NeV lines. The infrared region is dominated by a very strong He I 1083nm emission.Paper presented at the IAU Colloquium No. 93 on Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments, held at Dr. Remeis-Sternwarte Bamberg, F.R.G., 16–19 June, 1986.     

Evolution du spectre de HR Del de 1973 À 1979

Résumé De 1973 à 1979, on observe une diminution de l'intensité des raies d'émission et du continuum de HR Del au cours du temps.En 1978, on note la disparition des raies de haute excitation.La répartition énergétique spectrale dans le continu reste sensiblement la même dans l'intervalle 4000–5000 Å. Le fort excès ultraviolet trouvé de 3600 à 3250 Å est confirmé par les observations dans l'ultraviolet lointain effectuées à l'aide du satellite IUE.Nos observations montrent un important changement dans la structure des raies 4959 et 5007 Å de [Oiii] entre 1973 et 1976, les composantes polaires devenant plus faibles que les composantes équatoriales.

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From 1973 to 1979, the intensity of emission lines and continuum of HR Del has steadily diminished.High excitation lines have disappeared in 1978.The spectral energy repartition in the continuum remains the same in the spectral range 4000–5000 Å. The strong ultraviolet excess found in the spectral range 3600–3250 Å is confirmed by IUE satellite observations in the ultraviolet.Our observations show an important change in the structure of the [Oiii] lines 4959 and 5007 Å between 1973 and 1976, the polar components becoming weaker than the equatorial ones.

     

Evolution du spectre de la Nova Delphini 1967 en 1971 et 1972

Continued spectroscopic observations of Nova Del 67 during 1971 and 1972 show a general decrease of the nebular and coronal emission with respect to the local continuum. The continuous spectrum exhibits a strong Balmer emission (figure 1). Equivalent widths of Hi, Hei, Heii, Oi, [Oi], Oii, [Oii], Oiii, [Oiii], Niii, [Sii], [Aiii], [Neiii], [Nev], [Fevi], [Fevii], [Fex], [Fexi], [Fexiv], [Nixvi], [Nixv] are listed in tables 1 and 2.Figures 5 to 10 show several line profiles, which can be interpreted in terms of a model proposed by Hutchings (1972). Kinematical properties of the nova envelope do not seem to have changed in the 1968–1972 time interval. However, a study of the [Oiii] (4959 Å) line indicates that the physical conditions in the polar blobs in 1972 (T _e=10 660 K,N _e=5,5×10⁵ cm^–3) are different from those prevailing in equatorial rings (T _e=9×100 K,N _e=7×10⁵ cm^–3).

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Le matérial d'observation utilisé pour cette étude a été obtenu à l'aide de téléscopes de 120 cm, 152 cm et 193 cm de l'Observatoire de Haute-Provence (CNRS).     

Observations spectroscopiques de HD 50138

Observations of the Be star HD 50138 have been extended to the photographic infrared region up to 9500 Å. The main features noted in this wavelength range are strong lines of Oi (8446 Å), Hi (from P 9 to P 20), the Caii infrared triplet and the 8629 line attributed to Ni. The 7772 multiplet of Oi is shown to undergo important changes during the period of observations (1959–1971). Higher Balmer lines do not exhibit any emission component, but their profiles are variable and indicate the presence of satellite absorption, as already mentioned by some authors.Les observations ont été obtenues aux télescopes de 120 et 193 cm de l'observatoire de Haute-Provence (CNRS).