New models for the rapid evolution of the central star of the Stingray Nebula
arXiv:2104.00733 · doi:10.1093/mnras/stab890
Abstract
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\odot and 2.0 M\odot 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 1980s sudden mass loss episode, the sudden decline in mass loss, and the nebular recombination and fading.
22 pages, 11 figures, accepted in MNRAS
References in corpus (4)
- The Helium abundance and Delta Y / Delta Z in Lower Main Sequence stars
- Fe emission and ionized excess absorption in the luminous quasar 3C109 with XMM-Newton
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Cited by in corpus (4)
- Evolution of Hen\,3-1357, the Stingray Nebula
- Recombination of hot ionized nebulae: The old planetary nebula around V4334 Sgr (Sakurai's star)
- A primer on the formation and evolution of hydrogen deficient Central Stars of Planetary Nebulæ and Related Objects
- Pre-explosion helium shell flash in type Ia supernovae