Abstract:
We present a study of the high-resolution optical spectrum for the hot post-asymptotic giant
branch (post-AGB) star, Hen 3−1013, identified as the optical counterpart of the infrared source
IRAS 14331−6435. For the first time, the detailed identifications of the observed absorption
and emission features in the wavelength range 3700–9000 Å is carried out. Absorption lines
of H I, He I, C I, N I, O I, Ne I C II, N II, O II, Si II, S II, Ar II, Fe II, Mn II, Cr II, Ti II, Co II, Ni II,
S III, Fe III, and S IV were detected. From the absorption lines, we derived heliocentric radial
velocities of Vr = −29.6 ± 0.4 km s−1. We have identified emission permitted lines of O I,
N I, Fe II, Mg II, Si II, and Al II. The forbidden lines of [N I], [Fe II], [CrII], and [Ni II] have been
identified also. Analysis of [Ni II] lines in the gaseous shell gives an estimate for the electron
density Ne ∼ 107 cm−3 and the expansion velocity of the nebula Vexp = 12 km s−1. The mean
radial velocity as measured from emission features of the envelope is Vr = −36.0 ± 0.4 km s−1.
The Balmer lines H α, H β, and H γ show P Cyg behaviour which indicate ongoing post-AGB
mass loss. Based on ASAS and ASAS-SN data, we have detected rapid photometric variability
in Hen 3−1013 with an amplitude up to 0.2 mag in the V band. The star’s low-resolution
spectrum underwent no significant changes from 1994 to 2012. Based on archival data, we
have traced the photometric history of the star over more than 100 yr. No significant changes
in the star brightness have been found.
