New Models for the Central Star of the Stingray Nebula
<jats:title>Abstract/jats:title <jats:p>We present stellar evolution calculations from the Asymptotic Giant Branch (AGB) to the Planetary Nebula (PN) phase for models of initial mass 1.2 M⊙ and 2.0 M⊙ that experience a Late Thermal Pulse (LTP), a helium shell flash that occurs following the AGB and causes a rapid looping evolution between the AGB and PN phase. We use these models to make comparisons to the central star of the Stingray Nebula, V839 Ara (SAO 244567). The central star has been observed to be rapidly evolving (heating) over the last 50 to 60 years and rapidly dimming over the past 20–30 years. It has been reported to belong to the youngest known planetary nebula, now rapidly fading in brightness. In this paper we show that the observed timescales, sudden dimming, and increasing Log(g), can all be explained by LTP models of a specific variety. We provide a possible explanation for the nebular ionization, the 1980’s sudden mass loss episode, the sudden decline in mass loss, and the nebular recombination and fading./jats:p
This is a pre-copyedited, author-produced PDF of an article accepted for publication in 'Monthly Notices of the Royal Astronomical Society' following peer review. The version of record [Lawlor, T.M. (2021). New models for the rapid evolution of the central star of the Stingray Nebula. Monthly Notices of the Royal Astronomical Society.] is available online at: https://doi.org/10.1093/mnras/stab890.
|Work Title||New Models for the Central Star of the Stingray Nebula|
|License||In Copyright (Rights Reserved)|
|Publication Date||March 31, 2021|
|Publisher Identifier (DOI)||
|Deposited||January 13, 2022|
This resource is currently not in any collection.