Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (419) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (2)
· Also-Read Articles (Reads History)
· Translate This Page
On the evolution of those nuclei of planetary nebulae that experience a final helium shell flash
Iben, I., Jr.; Kaler, J. B.; Truran, J. W.; Renzini, A.
AA(Illinois, University, Urbana, IL), AB(Illinois, University, Urbana, IL), AC(Illinois, University, Urbana, IL), AD(Bologna, Università, Bologna, Italy)
Astrophysical Journal, Part 1, vol. 264, Jan. 15, 1983, p. 605-612. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Planetary Nebulae, Stellar Envelopes, Stellar Evolution, White Dwarf Stars, Abundance, Helium, Hertzsprung-Russell Diagram, Hydrogen, Stellar Luminosity, Stellar Winds, Thermonuclear Reactions
Bibliographic Code:


The authors suggest that some of the central stars of planetary nebulae experience a final thermal pulse after having achieved a white dwarf configuration and begun their descent along a cooling white dwarf sequence of nearly constant radius. Theoretical calculations show that there are two possible paths for the evolution of a PN nucleus past the final thermal pulse. In the first case, the pulse occurs well up on the white dwarf cooling track while the star is surrounded by a visible planetary nebula. The subsequent giant phase is of too short a duration to be observable, and the star next appears on the high-luminosity portion of the quiescent helium-burning track, where it may be identified with the nuclei of planetaries like Abell 30 and Abell 78. In the second case, the pulse occurs farther down on the track, when the surrounding nebulae would no longer be visible on existing surveys. The star remains longer in its giant state, where it is identified with the R CrB stars. Eventually, both of these fade to become non-DA white dwarfs.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences

More Article Retrieval Options

HELP for Article Retrieval

Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)


Find Similar Abstracts:

Use: Authors
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
arXiv e-prints