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)
· On-line Data
· References in the article
· Citations to the Article (57) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (1)
· NED Objects (1)
· Also-Read Articles (Reads History)
· Translate This Page
The discovery of nonradial instability strips for hot, evolved stars
Starrfield, S. G.; Cox, A. N.; Hodson, S. W.; Pesnell, W. D.
AA(Los Alamos National Laboratory, Los Alamos, NM; Arizona State University, Tempe, AZ), AB(Los Alamos National Laboratory, Los Alamos, NM), AC(Los Alamos National Laboratory, Los Alamos, NM), AD(Los Alamos National Laboratory, Los Alamos, NM; Florida, University, Gainesville, FL)
Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 268, May 1, 1983, p. L27-L32. Research supported by the U.S. Department of Energy. (ApJL Homepage)
Publication Date:
NASA/STI Keywords:
Abundance, Hot Stars, Stellar Envelopes, Stellar Evolution, Stellar Oscillations, Variable Stars, Blue Stars, Gas Ionization, Helium, Hertzsprung-Russell Diagram, Nonadiabatic Theory, Nuclear Reactions, Oxygen Isotopes, Stellar Models
Bibliographic Code:


Three different interior compositions are used in the present radial and nonradial, linear, nonadiabatic pulsation analyses of model stellar envelopes in the effective temperature range of 80,000-150,000 K, with total masses of 0.6 solar masses and radii chosen so that they line up along a prewhite dwarf cooling curve: (1) 100 percent C; (2) 50 percent C-12 and 50 percent O-16 by mass; and (3) 10 percent C-12 and 90 percent O-16 by mass. Radial and nonradial instability strips are found for each composition, caused the partial ionization of C, or O, or both. Attention is given to the cause of the pulsations of the hot, evolved star PG 1159-035, which, although perhaps too hot to lie within the proposed instability strips, is in some measure of agreement with models having significant amounts of O-16 near the stellar surface. This implies a greater production of O-16 through He burning than previously supposed.

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