Structure and clumping in the fast wind of NGC6543

TL;DR

This study uses far-UV spectroscopy to analyze the structure and clumping in the fast stellar wind of NGC6543, revealing episodic features similar to those in massive stars and implications for mass-loss rate estimates.

Contribution

It provides the first detailed analysis of wind clumping and episodic features in a planetary nebula central star using time-series UV spectroscopy and advanced modeling.

Findings

Detection of episodic optical depth enhancements in PV lines.

Identification of features similar to discrete absorption components in massive stars.

Clumping sensitivity observed in PV line profiles.

Abstract

Far-UV spectroscopy from the FUSE satellite is analysed to uniquely probe spatial structure and clumping in the fast wind of the central star of the H-rich planetary nebula NGC6543 (HD164963). Time-series data of the unsaturated PV 1118, 1128 resonance line P Cygni profiles provide a very sensitive diagnostic of variable wind conditions in the outflow. We report on the discovery of episodic and recurrent optical depth enhancements in the PV absorption troughs, with some evidence for a 0.17-day modulation time-scale. SEI line-synthesis modelling is used to derive physical properties, including the optical depth evolution of individual `events'. The characteristics of these features are essentially identical to the `discrete absorption components' (DACs) commonly seen in the UV lines of massive OB stars. We have also employed the unified model atmosphere code CMFGEN to explore spectroscopic signatures of clumping, and report in particular on the clear sensitivity of the PV lines to the clump volume filling factor. The results presented here have implications for the downward revision of mass-loss rates in PN central stars. We conclude that the temporal structures seen in the PV lines of NGC6543 likely have a physical origin that is similar to that operating in massive, luminous stars, and may be related to near-surface perturbations caused by stellar pulsation and/or magnetic fields.