Hostname: page-component-745bb68f8f-hvd4g Total loading time: 0 Render date: 2025-01-27T07:12:15.579Z Has data issue: false hasContentIssue false
  • English
  • Français

Light and velocity variability in Proto-Planetary Nebulae

Published online by Cambridge University Press:  25 May 2016

Bruce J. Hrivnak  and
Wenxian Lu
Bruce J. Hrivnak
Affiliation:
Valparaiso University, Valparaiso
Wenxian Lu
Affiliation:
Valparaiso University, Valparaiso

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We have been carrying out a program of monitoring light and velocity variability in proto-planetary nebulae (PPN). Variability might arise due to binarity or pulsation. Many planetary nebulae display a bipolar shape, and it is suggested that this is caused by binarity. This can be investigated in PPN, particularly by radial velocity studies of those of spectral types F and G. Pulsation is known to exist in other types of post-AGB stars, and can be a means to learn more about the physical properties of the stars. No previous study of a sample of PPN has been published.

Type
V. From AGB to Planetary Nebulae
Information
Symposium - International Astronomical Union , Volume 180: Planetary Nebulae , 1997 , pp. 351
Copyright
Copyright © Kluwer 1997