Physical and Chemical Properties of Planetary Nebulae with WR-type Nuclei

TL;DR

This study analyzes the physical and chemical properties of planetary nebulae with Wolf-Rayet nuclei using spectroscopic data, revealing correlations between abundance discrepancies, temperature variations, and nebular evolution.

Contribution

It provides new insights into the plasma diagnostics and elemental abundances in planetary nebulae with WR-type nuclei, highlighting the role of H-deficient materials.

Findings

Abundance discrepancy factors are correlated with temperature dichotomies.

H-deficient materials are embedded in the nebulae.

Surface brightness relates to nebular evolution.

Abstract

We have carried out optical spectroscopic measurements of emission lines for a sample of Galactic planetary nebulae with Wolf-Rayet (WR) stars and weak emission-line stars (wels). The plasma diagnostics and elemental abundance analysis have been done using both collisionally excited lines (CELs) and optical recombination lines (ORLs). It is found that the abundance discrepancy factors (ADF=ORL/CEL) are closely correlated with the dichotomy between temperatures derived from forbidden lines and those from He I recombination lines, implying the existence of H-deficient materials embedded in the nebula. The H$\beta$ surface brightness correlations suggest that they might be also related to the nebular evolution.