X-ray emission from jet-wind interaction in planetary nebulae

Muhammad Akashi*, Yohai Meiron, Noam Soker

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

19 Scopus citations

Abstract

We conduct 2D numerical simulations of jets expanding into the slow wind of asymptotic giant branch stars. We show that the post-shock jets' material can explain the observed extended X-ray emission from some planetary nebulae (PNs). Such jets are thought to shape many PNs, and therefore it is expected that this process will contribute to the X-ray emission from some PNs. In other PNs (not simulated in this work) the source of the extended X-ray emission is the shocked spherical wind blown by the central star. In a small fraction of PNs both sources might contribute, and a two-temperatures gas will fit better the X-ray properties than a one-temperature gas. A spatial separation between these two components is expected.

Original languageEnglish
Pages (from-to)563-568
Number of pages6
JournalNew Astronomy
Volume13
Issue number8
DOIs
StatePublished - Nov 2008
Externally publishedYes

Keywords

  • ISM: jets and outflows
  • ISM: planetary nebulae: general
  • Stars: mass loss
  • X-rays: ISM

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