Nonthermal radio emission from planetary nebulae

Ruth Dgani*, Noam Soker

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

13 Scopus citations

Abstract

In a recent analysis of the radio emission from the planetary nebula A30, Dgani, Evans, & White claim that the emission, located in the inner region, is probably dominated by nonthermal emission. We propose a model to explain this. We assume that the fast wind, blown by the central star of A30, carries a very weak magnetic field. The interaction of this wind with a cluster of dense condensations traps the magnetic field lines for a long time and stretches them, leading to a strong magnetic field. If relativistic particles are formed as the fast wind is shocked, then the enhanced magnetic field will result in nonthermal radio emission. The typical nonthermal radio flux at 1 GHz can be up to several millijanskys. In order to detect the nonthermal emission, the emitting region should be spatially resolved from the main optical nebula. We list other planetary nebulae that may possess nonthermal radio emission.

Original languageEnglish
Pages (from-to)L83-L86
JournalAstrophysical Journal
Volume499
Issue number1 PART II
DOIs
StatePublished - 1998
Externally publishedYes

Keywords

  • ISM: kinematics and dynamics
  • ISM: magnetic fields
  • Planetary nebulae: general
  • Planetary nebulae: individual (A30)
  • Radio continuum: ISM

Fingerprint Dive into the research topics of 'Nonthermal radio emission from planetary nebulae'. Together they form a unique fingerprint.

Cite this