An analysis of the optical spectra of the post-asymptotic giant branch stars LSIV -12 111 and HD 341617

Details An analysis of the optical spectra of the post-asymptotic giant branch stars LSIV -12 111 and HD 341617 An analysis of the optical spectra of the post-asymptotic giant branch stars LSIV -12 111 and HD 341617

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...401.1119r&link_type=abstract

Astronomy and Astrophysics, v.401, p.1119-1129 (2003)

Astronomy and Astrophysics

Astrophysics

32

Stars: Abundances, Stars: Supergiants, Stars: Early-Type, Stars: Fundamental Parameters

Scientific paper

High spectral resolution and signal-to-noise observations of the absorption and emission line spectra in two post-asymptotic-giant-branch (PAGB) stellar candidates, LSIV -12 111 and HD 314617 are discussed. The absorption line spectra have been analysed using non-LTE model atmosphere techniques to determine stellar atmospheric parameters and chemical compositions, both in absolute terms and relative to a standard star, HD 13841. The atmospheric parameters differ from previous estimates based on LTE model atmospheres, probably due to non-LTE effects. In turn these imply stellar masses that are generally larger than have been previously estimated. Both PAGB candidates have relative uniform underabundances of metals with mean values of -0.35 dex for LSIV -12 111 and -0.50 dex for HD 314617.
Furthermore, their abundance patterns are remarkably similar to that observed for optically bright, F-type PAGBs. From the emission spectra, the plasma parameters and angular size of the circumstellar material are constrained, and these are consistent with previous estimates and with a PAGB evolutionary stage.

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