Changes in the spectrum of the recombining planetary nebula He 1-5

Details Changes in the spectrum of the recombining planetary nebula He 1-5 Changes in the spectrum of the recombining planetary nebula He 1-5

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009astl...35..633a&link_type=abstract

Astronomy Letters, Volume 35, Issue 9, pp.633-637

Astronomy and Astrophysics

Astronomy

Scientific paper

In 2008, we observed the spectrum of the planetary nebula He 1-5, which has had no ionization source for more than 50 years. Comparison with the observations performed in 1972-1976 and 1988 shows that the line intensity ratio I( λ5007[O III])/ I(H β) decreased by a factor of 2.5, the intensity ratio of the red [N II] doublet to H α was almost constant, and the [S II]-to-H α intensity ratio may have slightly increased. The observed changes in the spectrum agree, within the limits of the observational errors, with the calculations of gas recombination in a medium-excitation nebula performed by Tylenda in 1980, but the nitrogen line intensities are higher than the calculated ones by 10-15%. This is most likely related to the slightly reduced nitrogen abundance adopted in the model. The onset of nebular recombination dates from the end of the 19th century and is consistent with its estimate from the photometric history of the central star.

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