EDP Sciences
Free Access
Issue
A&A
Volume 392, Number 1, September II 2002
Page(s) 143 - 150
Section Formation, structure and evolution of stars
DOI https://doi.org/10.1051/0004-6361:20020909
Published online 22 August 2002


A&A 392, 143-150 (2002)
DOI: 10.1051/0004-6361:20020909

Discovery of spectral variation in the optical counterpart of IRAS 01005+7910

V. G. Klochkova1, 2, M. V. Yushkin1, 2, A. S. Miroshnichenko3, 4, V. E. Panchuk1, 2 and K. S. Bjorkman3

1  Special Astrophysical Observatory of the Russian Academy of Sciences, Karachai-Cirkassian Republic, Nizhnij Arkhyz 369167, Russia
2  Isaac Newton Institute of Chile, SAO Branch
3  Ritter Observatory, Dept. of Physics & Astronomy, University of Toledo, Toledo, OH 43606-3390, USA
4  Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo, 196140 Saint-Petersburg, Russia

(Received 1 March (2002) / Accepted 29 May (2002) )

Abstract
We present a study of the high-resolution spectroscopic data for the proto-planetary nebula candidate IRAS 01005+7910. For the first time a careful spectral line identification is carried out, and a significant variability of the optical spectrum is detected. We found absorption lines of C II/III, N II, O II, Al III, Si III, and Mg II ( $\lambda4481$ Å), as well as emission lines of Si II and [Fe II]. Both absorption and emission components are present in the Balmer lines, Na I resonance D 1,2 lines, He I, and Fe III lines. The He I line profiles vary from straight to inverse P Cyg-type on a timescale of days to months. The resonance Na I lines show 5 absorption components at a resolution of $R=60\,000$. Additionally, the Na I D 2 line exhibits a variable emission component with a width comparable to that of the Balmer line emission components. Using the model atmospheres method within the LTE-approximation, the effective temperature ( $T_\mathrm{eff}\sim21\,500$ K), the metallicity $\mathrm{[Fe/H]}_\odot=-0.31$, and the ratio C/O>1 is reported. Finally, we suggest that IRAS 01005+7910 is a carbon-rich post-AGB star with a luminosity $\log(L/L_\odot)=3.6$ at a distance about 3 kpc.


Key words: stars: evolution -- stars: AGB and post-AGB -- stars: emission-line -- stars: individual: IRAS 01005+7910 -- techniques: spectroscopic

Offprint request: V. G. Klochkova, valenta@sao.ru

SIMBAD Objects



© ESO 2002

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.