| Issue |
A&A
Volume 422, Number 2, August I 2004
|
|
|---|---|---|
| Page(s) | 637 - 650 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361:20035592 | |
| Published online | 09 July 2004 | |
Optical and infrared spectroscopic analysis of the post-AGB star candidate IRAS 19386+0155 *
1
Observatório Nacional, Rua José Cristino, 77, CEP 20921-400, São Cristóvão, Rio de Janeiro, Brazil e-mail: claudio@on.br
2
GEMAC/Departamento de Astronomia/Observatório do Valongo/UFRJ, Ladeira Pedro Antônio 43, CEP 20080-090, Rio de Janeiro, Brazil
Received:
29
October
2003
Accepted:
24
March
2004
This work reports high-resolution spectroscopic stellar
parameters and abundance analysis of the post-AGB star IRAS 19386+0155. The analysis of the high resolution spectrum shows that it
has an effective temperature of 
K and a
surface gravity of log 
. The abundance analysis
reveals IRAS 19386+0155 to be a metal-poor object having
![$\rm [Fe/H]=-1.1$](/articles/aa/abs/2004/29/aa0592/aa0592_tex_eq3.png)
. Carbon, oxygen and nitrogen are found to be slight
underabundant than solar, and so are the α-elements (Mg, Si and Ca). The analysis of ISO spectra revealed an oxygen-rich envelope and
showed crystalline silicate features. The dust envelope of this
object was modelled using a Monte Carlo type numerical method and
amorphous and crystalline silicate grains were considered. The
photospheric temperature obtained through the optical spectroscopy was
used to constrain these models. The Spectral Energy Distribuition
(SED) of this object is broad and extensive suggesting the presence of
a dust disk around IRAS 19386+0155.
Key words: stars: AGB and post / AGB / stars: abundances
Based on observations made with the 1.52 m telescope at the European Southern Observatory (La Silla, Chile) under the agreement with the CNPq-Observatório Nacional (Brazil) Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the UK) and with the participation of ISAS and NASA.
© ESO, 2004
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