On the variations of O III forbidden line intensities in the spectrum of the planetary nebula IC 4997

Details On the variations of O III forbidden line intensities in the spectrum of the planetary nebula IC 4997 On the variations of O III forbidden line intensities in the spectrum of the planetary nebula IC 4997

Oct 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997azh....74..678e&link_type=abstract

Astronomicheskij Zhurnal, vol. 74, p. 678

Astronomy and Astrophysics

Astronomy

Planetary Nebulae, Oxygen Spectra, Forbidden Bands, Stellar Winds, Line Spectra, High Temperature Plasmas, Astronomical Spectroscopy, Oxygen Ions, Electron Density Profiles

Scientific paper

The causes of asynchronous variations in the intensities of forbidden O III lines in the spectrum of the planetary nebula IC 4997 are considered. It is shown that the strengthening of the 4363-A line with a simultaneous weakening of the N1 and N2 lines can be explained by a severalfold increase of the mass-loss rate from the nucleus, up to 1-2 x 10 exp -7 solar mass/yr, over several years. The ionization model of the nebula under the combined effect of nucleus emission and the emission from a variable hot stellar wind with electron temperature of 500,000 K is used to calculate the theoretical line intensities. The calculations included 12 levels of O III. In the region of O III line formation, the electron density of 10 exp 6/cu cm and Te, which varies from 12,000 to 15,000 K, yield theoretical line intensities that are in best agreement with observations. The X-ray luminosity of the stellar wind from the nucleus at energies not less than 0.2 keV is on the order of 10 exp 35 erg/s, but the interstellar extinction rules out the possibility of observing this object.

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