Abundances of Planetary Nebula M1-42

TL;DR

This study reanalyzed the planetary nebula M1-42 using infrared and other spectral data to accurately determine its chemical composition, revealing unusually high abundances of certain elements and insights into its stellar evolution.

Contribution

It provides a revised chemical composition of M1-42 based on infrared spectral analysis, highlighting differences from previous results and implications for stellar evolution.

Findings

High neon, argon, and sulfur abundances compared to other planetary nebulae.

Evidence of second dredge-up and hot bottom burning in the progenitor star.

Central star's temperature and luminosity suggest a more massive original star.

Abstract

The spectra of the planetary nebula M1-42 is reanalysed using spectral measurements made in the mid-infrared with the Spitzer Space Telescope. The aim is to determine the chemical composition of this object. We also make use of ISO, IUE and ground based spectra. Abundances determined from the mid- and far-infrared lines, which are insensitive to electron temperature, are used as the basis for the determination of the composition, which are found to substantially differ from earlier results. High values of neon, argon and sulfur are found. They are higher than in other PN, with the exception of NGC6153, a nebula of very similar abundances. The high values of helium and nitrogen found indicate that the second dredge-up and hot bottom burning has occurred in the course of evolution and that the central star was originally more massive than 4Msun. The present temperature and luminosity of the central star is determined and at first sight may be inconsistent with such a high mass.