A search for Type Ia supernova progenitors: the central stars of the planetary nebulae NGC 2392 and NGC 6026

TL;DR

This study uses photoionization modeling to evaluate whether the central stars of NGC 2392 and NGC 6026 could be close binary systems capable of producing Type Ia supernovae, based on their total masses.

Contribution

It provides the first detailed assessment of the binary nature and mass estimates of these planetary nebulae's central stars as potential SN Ia progenitors.

Findings

NGC 2392 likely has a massive white dwarf companion with a total mass of ~1.6 Ms

NGC 6026 has a total mass of ~1.1 Ms and is not a SN Ia progenitor

NGC 2392's system is a promising candidate for SN Ia progenitor studies

Abstract

We use photoionization modeling to assess the binary nature of the central stars of NGC 2392 and NGC 6026. If they are close binaries, they are potential Type Ia supernova (SN Ia) progenitors if the total mass exceeds the Chandrasekhar limit. We show that the nucleus of NGC 2392 likely has a hot, massive (\simeq 1 Ms) white dwarf companion, and a total mass of ~ 1.6 Ms, making it an especially interesting system. The binary mass in NGC 6026 is less, ~ 1.1 Ms. Even though its orbital period is short, it is not considered to be a SN Ia progenitor.