2010A&A...517A...6L


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.11CEST10:06:21

2010A&A...517A...6L - Astronomy and Astrophysics, volume 517, A6-6 (2010/7-1)

Abundance analysis for long period variables. Velocity effects studied with O-rich dynamic model atmospheres.

LEBZELTER T., NOWOTNY W., HOEFNER S., LEDERER M.T., HINKLE K.H. and ARINGER B.

Abstract (from CDS):

Measuring the surface abundances of AGB stars is an important tool for studying the effects of nucleosynthesis and mixing in the interior of low- to intermediate mass stars during their final evolutionary phases. The atmospheres of AGB stars can be strongly affected by stellar pulsation and the development of a stellar wind, though, and the abundance determination of these objects should therefore be based on dynamic model atmospheres. We investigate the effects of stellar pulsation and mass loss on the appearance of selected spectral features (line profiles, line intensities) and on the derived elemental abundances by performing a systematic comparison of hydrostatic and dynamic model atmospheres. High-resolution synthetic spectra in the near infrared range were calculated based on two dynamic model atmospheres (at various phases during the pulsation cycle) as well as a grid of hydrostatic COMARCS models with effective temperatures Teff and surface gravities logg over an adequate range. Equivalent widths of a selection of atomic and molecular lines (Fe, OH, CO) were derived in both cases and compared with each other. In the case of the dynamic models, the equivalent widths of all investigated features vary over the pulsation cycle. A consistent reproduction of the derived variations with a set of hydrostatic models is not possible, but several individual phases and spectral features can be reproduced well with the help of specific hydrostatic atmospheric models. In addition, we show that the variations in equivalent width that we found on the basis of the adopted state-of-the-art dynamic model atmospheres agree qualitatively with observational results for the Mira RCas over its light cycle. The findings of our modelling form a starting point to deal with the problem of abundance determination in strongly dynamic AGB stars (i.e., long-period variables). Our results illustrate that some quantities such as the C/O ratio can probably still be determined to a reasonable accuracy, but the measurement of other quantities will be hampered by the dynamics. The qualitative agreement with observations of RCas opens promising possibilities for a forthcoming quantitative comparison of our synthetic spectra with observed ones of AGB variables in the globular cluster 47 Tuc.

Abstract Copyright:

Journal keyword(s): stars: late-type - stars: AGB and post-AGB - stars: atmospheres - stars: abundances - line: profiles

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 104 GlC 00 24 05.359 -72 04 53.20   5.78 4.09     ~ 3548 0
2 Cl* NGC 104 SAW V5 V* 00 25 03.6658607985 -72 09 31.685961205   12.44 11.44     M2II/III 24 0
3 Cl* NGC 104 SAW V3 Mi* 00 25 15.9991520189 -72 03 54.667782644   13.50 11.51     M2/3Ib-IIe 35 0
4 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5669 1
5 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2134 0
6 V* R Cas Mi* 23 58 24.8700291935 +51 23 19.691977266 6.71 6.63 4.80     M6.5-9e 677 0

    Equat.    Gal    SGal    Ecl

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2020.07.11-10:06:21

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