Hostname: page-component-cd9895bd7-dk4vv Total loading time: 0 Render date: 2024-12-26T17:47:06.260Z Has data issue: false hasContentIssue false
  • English
  • Français

Lower Limit for NPN's Masses

Published online by Cambridge University Press:  19 July 2016

Amos Harpaz
Amos Harpaz*
Affiliation:
Department of Physics, the Technion, Haifa 32000, Israel

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.

The lowest mass observed for a nucleus of a planetary nebula (NPN) is about 0.55 M⊙ (Weidemann and Koester, 1983, Schonberner, 1983). Hence, Lower mass WD's should have been produced without going through the phase of a visible PN ejection. Recently, Harpaz et al. (1987), have shown that very low mass WD's (up to 0.45 M⊙) can be formed by a single star evolution from red giant branch (RGB) stars, due to mass loss along the RGB. It turns out that WD's in mass range of 0.46–0.55 M⊙ formed by a single star evolution should be formed from the AGB, without an observable PN.

Type
V. Origin of Planetaries
Information
Symposium - International Astronomical Union , Volume 131: Planetary Nebulae , 1989 , pp. 454
Copyright
Copyright © Kluwer 1989 

References

Harpaz, A., Kovetz, A., 1981, Astron. Astrophys., 93, 200.Google Scholar
Harpaz, A., Kovetz, A., Shaviv, G., 1987, Astrophys. J., in press.Google Scholar
Schonberner, D., 1983, Astrophys. J., 272, 708.CrossRefGoogle Scholar
Wei demann, V., Koester, D., 1983, Astron. Astrophys., 121, 77 Google Scholar