The origin and shaping of planetary nebulae: Putting the binary hypothesis to the test

Orsola De Marco*

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

227 Citations (Scopus)
14 Downloads (Pure)

Abstract

Planetary nebulae (PNs) are circumstellar gas ejected during an intense mass-losing phase in the lives of asymptotic giant branch stars. PNs have a stunning variety of shapes, most of which are not spherically symmetric. The debate over what makes and shapes the circumstellar gas of these evolved, intermediate mass stars has raged for two decades. Today the community is reaching a consensus that single stars cannot trivially manufacture PNs and impart to them nonspherical shapes and that a binary companion, possibly even a substellar one, might be needed in a majority of cases. This theoretical conjecture has, however, not been tested observationally. In this review we discuss the problem from both the theoretical and observational standpoints, explaining the obstacles that stand in the way of a clean observational test and ways to ameliorate the situation. We also discuss indirect tests of this hypothesis and its implications for stellar and galactic astrophysics.

Original languageEnglish
Pages (from-to)316-342
Number of pages27
JournalPublications of the Astronomical Society of the Pacific
Volume121
Issue number878
DOIs
Publication statusPublished - Apr 2009
Externally publishedYes

Bibliographical note

Copyright 2009 by University of Chicago Press. Originally published in Publications of the Astronomical Society of the Pacific.

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