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The Chemical Composition of Post AGB Stars

Published online by Cambridge University Press:  07 August 2017

M. Parthasarathy ,
P. Garcia Lario  and
S.R. Pottasch
M. Parthasarathy
Affiliation:
Indian Institute of Astrophysics, Bangalore 560034, India
P. Garcia Lario
Affiliation:
Laboratorio de Astrofisica Espacial Y Fisica Fundamental, Estacion de Villafranca del Castillo, Apartado de Correos 50727, E-28080 Madrid, Spain
S.R. Pottasch
Affiliation:
Kapteyn Astronomical Institute, Postbus 800, Nl-9700 AV Groningen, The Netherlands

Extract

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The F-type supergiant HD 56126 (F5I) is an IRAS source with detached cold dust shell with characteristics similar to the dust shells around planetary nebulae. From an analysis of high resolution and high signal to noise ratio spectra metal and CNO abundances have been determined. It is found that in HD 56126 [C/H] =−0.01, [N/H]=+0.17, [O/H] = −0.02, [S/H]=+0.01 and [Fe/H]< −1.0. The C/N/O abundance ratios and CNO abundances relative to Fe of HD 56126 and related post AGB stars suggest that they have on their photospheres the material processed by triple alpha, CN and ON cycles.

Type
IV. Planetary Nebulae Connection: Evolution from the AGB
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 352
Copyright
Copyright © Kluwer 1993