Physical conditions and chemical abundances of the variable planetary nebula IC 4997

The planetary nebula (PN) IC 4997 is one of a few rapidly evolving objects with variable brightness and nebular emission around a hydrogen-deficient star. In this study, we have determined the physical conditions and chemical abundances of this object using the collisionally excited lines (CELs) and optical recombination lines (ORLs) measured from the medium-resolution spectra taken in 2014 July with the FIbre-fed echelle Spectrograph on the Nordic Optical Telescope at La Palma Observatory. We derived electron densities of greater than or similar to 3 x 10(4) cm(-3) and electron temperatures of greater than or similar to 14 000 K from CELs, whereas cooler temperatures of similar to 11 000 and similar to 7000 K were obtained from helium and heavy element ORLs, respectively. The elemental abundances deduced from CELs point to a metal-poor progenitor with [O/H] less than or similar to -0.75, whereas the ORL abundances are slightly above the solar metallicity, [O/H] approximate to 0.15. Our abundance analysis indicates that the abundance discrepancy factors (ADFs equivalent to ORLs/CELs) of this PN are relatively large: ADF(O2+) greater than or similar to 8 and ADF(N2+) greater than or similar to 7. Further research is needed to find out how the ADFs and variable emissions are formed in this object and whether they are associated with a binary companion or a very late thermal pulse.

Automated summary

This study investigates the physical conditions and chemical abundances of the planetary nebula IC 4997. By analyzing spectral data, the electron densities, electron temperatures, and elemental abundances of this object are determined, revealing large abundance discrepancy factors. Further research is needed to understand the formation mechanisms of these discrepancy factors and variable emissions.