Accounting for planet-shaped planetary nebulae

Efrat Sabach, Noam Soker

Research output: Contribution to journalArticlepeer-review

12 Scopus citations

Abstract

By following the evolution of several observed exoplanetary systems, we showthat by lowering the mass-loss rate of single solar-like stars during their two giant branches, these stars will swallow their planets at the tip of their asymptotic giant branch (AGB) phase. This will most likely lead the stars to form elliptical planetary nebulae (PNe). Under the traditional mass-loss rate these stars will hardly form observable PNe. Stars with a lower mass-loss rate as we propose, about 15 per cent of the traditional mass-loss rate of single stars, leave the AGB with much higher luminosities than what traditional evolution produces. Hence, the assumed lower mass-loss rate might also account for the presence of bright PNe in old stellar populations. We present the evolution of four exoplanetary systems that represent stellar masses in the range of 0.9-1.3M. The justification for this low mass-loss rate is our assumption that the stellar samples that were used to derive the traditional average single-star mass-loss rate were contaminated by stars that suffer binary interaction.

Original languageEnglish
Pages (from-to)286-294
Number of pages9
JournalMonthly Notices of the Royal Astronomical Society
Volume473
Issue number1
DOIs
StatePublished - 1 Jan 2018
Externally publishedYes

Keywords

  • Binaries: close
  • Planetary systems
  • Stars:AGBand post-AGB
  • Stars:mass-loss

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