Variable Hα line emission from the central star of the Helix Nebula

Robert A. Gruendl, You Hua Chu, Ian J. O'Dwyer, Martín A. Guerrero

Research output: Contribution to journalArticle

Abstract

The central star of the Helix Nebula is a hot white dwarf with unexpected hard X-ray emission. With an effective temperature of ∼100,000 K, the star is a powerful source of H-ionizing radiation; the atmosphere of a stellar or planetary companion, if present, will be ionized and emit recombination lines. To probe the origin of hard X-ray emission from the Helix Nebula's central star, we have obtained multiepoch, high-dispersion spectra of the star and have found temporal variation in the Hα line profile over a time span of 1 week. The observed width and strength of the variable Hα emission component are consistent with the hypothesized dMe companion proposed to explain the hard X-ray emission. A dMe companion, however, cannot explain the possible detection of variable He II and [N II] emission. Follow-up spectroscopic monitoring of the Helix Nebula central star is needed to better establish the identification of the spectral lines and their temporal behavior in order to determine the origin of the optical variability and hard X-ray emission.

Original languageEnglish (US)
Pages (from-to)308-312
Number of pages5
JournalAstronomical Journal
Volume122
Issue number1
DOIs
StatePublished - Jul 1 2001

Keywords

  • Planetary nebulae: individual (NGC 7293)
  • Stars: activity
  • Stars: individual (WD 2226-210)
  • White dwarfs

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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