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Observed Bolometric Luminosities of Carbon Stars

Frogel, Jay A. and Cohen, Judith G. and Persson, S. E. and Elias, Jonathan H. (1981) Observed Bolometric Luminosities of Carbon Stars. In: Physical Processes in Red Giants. Astrophysics and Space Science Library. No.88. Springer Netherlands , Dordrecht, pp. 159-164. ISBN 9789400984943. https://resolver.caltech.edu/CaltechAUTHORS:20190529-161904668

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Abstract

To the best of our knowledge, most carbon stars are cool stars on their second ascent of the giant branch, i.e. the asymptotic giant branch. By some means they have mixed nuclear processed, carbon enriched material to their surfaces and probably have luminosities that are greater than those that mark the termination point of first time evolution up the giant branch, i.e. the location of the core helium flash. Observational and theoretical evidence for this picture may be found in Iben and Truran (1978), Renzini and Voli (1980), Scalo (1976), Richer, Olander and Westerlund (1979), and earlier references these authors cite.


Item Type:Book Section
Related URLs:
URLURL TypeDescription
https://doi.org/10.1007/978-94-009-8492-9_15DOIArticle
ORCID:
AuthorORCID
Cohen, Judith G.0000-0002-8039-4673
Additional Information:© D. Reidel Publishing Company 1981. We are very grateful to Victor Blanco, Martin McCarthy, and Betty Blanco for supplying us with the results of their grism surveys before publication. Our program would have been impossible otherwise. JAF thanks Icko Iben and Alvio Renzini for several informative discussions.
Subject Keywords:Star Formation; Globular Cluster; Dwarf Galaxy; Luminosity Function; Asymptotic Giant Branch
Series Name:Astrophysics and Space Science Library
Issue or Number:88
Record Number:CaltechAUTHORS:20190529-161904668
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190529-161904668
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:95925
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:31 May 2019 16:03
Last Modified:03 Oct 2019 21:18

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