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

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

Nov 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974ap%26ss..31..169a&link_type=abstract

Astrophysics and Space Science, Volume 31, Issue 1, pp.169-185

Astronomy and Astrophysics

Astrophysics

6

Scientific paper

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 H i, He i, He ii, O i, [O i], O ii, [O ii], O iii, [O iii], N iii, [S ii], [A iii], [Ne iii], [Ne v], [Fe vi], [Fe vii], [Fe x], [Fe xi], [Fe xiv], [Ni xvi], [Ni xv] 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 [O iii] (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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