Péridier Library Abstract Archive
Abstract No. UT 333
Title: The Optical Spectrum of HR4049 (includes a line identification from 3650 to 10850 Å)
Author(s): Eric J. Bakker, Frank L.A. Van der Wolf, Henny J.G.L.M. Lamers, Austin F. Gulliver, Roger Ferlet, Alfred Vidal-Madjar
Keywords: line identification, line profiles, binaries: close, stars: chemical peculiar, stars: HR4049, stars: AGB and post-AGB
E-Mail: Eric J. Bakker (to request a full copy of this paper)
Preprint: 9509110 Document source or PostScript
Release date: 10/04/95 14:33:35
Publication status: accepted by A&A main journal
Comments: 21 pages, 9 figures
High-resolution optical spectra (UES/WHT)
of the extreme metal-poor post-AGB star HR4049 were obtained at
four different orbital phases. The spectra cover the wavelength
region from 3650 Å to 10850 Å at a resolution of
R = 5.2 x 104.
These observations are supplemented with four high-resolution spectra
of the NaI D1 & D2 and CaII K lines at R = 105 (CAT/CES).
The optical spectrum shows 217 spectral lines:
the Balmer series (H alpha-H35), the Paschen series (P9-P23), NI,
OI and numerous CI lines.
We show that the lines of H alpha, H beta, H gamma, and NaI D
show significant changes in profile between different observation
dates. Nine components were identified in the profile of the NaI D lines
of which three are circumstellar and six interstellar.
The stronger CI lines are asymmetric and we derive a post-AGB mass-loss
of Mdot = 6 ± 4 x 10-7 Msol / yr
from the asymmetry. The [OI] 6300 Å line has been detected in emission
at the system velocity and we argue that the emission is
from an almost edge-on disk with a radius of about 20 Rstar.