X-ray emission by a shocked fast wind from the central stars of planetary nebulae

Muhammad Akashi*, Noam Soker, Ehud Behar

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

12 Scopus citations


We calculate the X-ray emission from the shocked fast wind blown by the central stars of planetary nebulae (PNe) and compare with observations. Using spherically symmetric self-similar solutions, we calculate the flow structure and X-ray temperature for a fast wind slamming into a previously ejected slow wind. We find that the observed X-ray emission of six PNe can be accounted for by shocked wind segments that were expelled during the early-PN phase, if the fast wind speed is moderate, , and the mass-loss rate is a few times . We find, as proposed previously, that the morphology of the X-ray emission is in the form of a narrow ring inner to the optical bright part of the nebula. The bipolar X-ray morphology of several observed PNe, which indicates an important role of jets, rather than a spherical fast wind, cannot be explained by the flow studied here.

Original languageEnglish
Pages (from-to)1706-1716
Number of pages11
JournalMonthly Notices of the Royal Astronomical Society
Issue number4
StatePublished - Jun 2006
Externally publishedYes


  • Stars: mass-loss
  • Stars: winds, outflows
  • X-rays: ISM

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