The short orbital period binary star at the heart of the planetary nebula M 3-1

David Jones*, Henri M. J. Boffin, Paulina Sowicka, Brent Miszalski, Pablo Rodríguez-Gil, Miguel Santander-García, Romano L. M. Corradi

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

24 Citations (Scopus)

Abstract

We present the discovery of a 3h5m orbital-period binary star at the heart of the planetary nebula M 3-1 - the shortest period photometrically variable central star known and second only to V458 Vul, in general. Combined modelling of light and radial velocity curves reveals both components to be close to Roche lobe filling, strongly indicating that the central star will rapidly evolve to become a cataclysmic variable, perhaps experiencing a similar evolution to V458 Vul resulting in a nova eruption before the planetary nebula has fully dissipated. While the short orbital period and near Roche lobe filling natures of both components make the central binary of M 3-1 an important test case with which to constrain the formation processes of cataclysmic variables, novae, and perhaps even supernovae type Ia.
Original languageEnglish
Pages (from-to)L75-L79
Number of pages5
JournalMonthly Notices of the Royal Astronomical Society: Letters
Volume482
Issue number1
DOIs
Publication statusPublished - 1 Jan 2019
Externally publishedYes

Keywords

  • stars: AGB and post-AGB
  • binaries: eclipsing
  • binaries: spectroscopic
  • planetary nebulae: individual: PN G242.6 − 11.6
  • planetary nebulae: individual: M 3-1
  • binaries: close

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