A phenomenological model for the extended zone above AGB stars

Noam Soker*

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

11 Scopus citations

Abstract

I suggest the existence of an extended zone above the surface of asymptotic giant branch (AGB), as well as similar stars experiencing high mass-loss rates. In addition to the escaping wind, in this zone there are parcels of gas that do not reach the escape velocity. These parcels of dense gas rise slowly and then fall back. The wind and bound gas exist simultaneously to distances of ∼100AU. I term this region the effervescent zone. In this phenomenological study I find that the density of the bound material in the effervescent zone falls as ∼r-5/2, not much faster than the wind density. The main motivation to propose the effervescent model is to allow wide binary companions to influence the morphology of the descendant planetary nebulae (PN) by accreting mass from the effervescent zone. Accretion from the effervescent zone is more efficient than accretion from the wind in forming an accretion disk around the companion. The companion might then blow two jets that will shape the descendant PN.

Original languageEnglish
Pages (from-to)491-497
Number of pages7
JournalNew Astronomy
Volume13
Issue number7
DOIs
StatePublished - Oct 2008

Keywords

  • (ISM:) planetary nebulae: general
  • Stars: AGB and post-AGB
  • Stars: mass-loss
  • Stars: winds, outflows

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