A&A 367, 826-830 (2001)
DOI: 10.1051/0004-6361:20000496
E. Josselin1,2 - A. Lèbre2
1 -
Observatorio Astronómico Nacional (OAN), IGN, Apartado 1143,
28800 Alcalá de Henares, Spain
2 -
GRAAL-CC72, UMR 5024-ISTEEM, CNRS/Univ. Montpellier II, Place E. Bataillon,
34095 Montpellier Cedex, France
Received 25 April 2000 / Accepted 13 November 2000
Abstract
In spite of recent detailed studies, the nature of HD 179821
is still puzzling. It is classified either as an intermediate-mass
post-AGB star or as a massive supergiant. We present here new high
sensitivity radio observations of HD 179821
in the circumstellar 12CO and 13CO lines. We also report the
new detection of HCO+ in this object. The 12CO line intensities
allow estimations of the mass-loss rate of HD 179821 and of the dynamical
age of its circumstellar envelope. The comparison between 12CO and
13CO lines indicates an isotopic ratio for carbon of at most 5.
Such a low value is characteristic of (post-)AGB stars with low-mass
progenitors. Furthermore, the HCO+ molecular ion indicates that an
active photochemistry occurs in the envelope of HD 179821, probably
induced by UV photons emitted as the central post-AGB star warms up and/or
by shocks generated by interacting winds.
Key words: stars: AGB and post-AGB - stars: circumstellar matter - stars: individual: HD 179821
The post-Main Sequence evolution of stars is strongly dependent on their
initial mass. On the one hand, low- and intermediate-mass stars
(initial mass
)
evolve along the Red Giant
Branch (RGB) and Asymptotic Giant Branch (AGB) before becoming Planetary
Nebulae (PNe) (Habing 1996). The transition phase between AGB stars and
PNe, designed as the post-AGB phase or proto-PNe (PPNe) phase, is very
brief (
103 yrs, Blöcker 1995), but its study is a clue to
understand the shaping of PNe and the properties of their central stars (Kwok 1993).
On the other hand, massive stars (
-10
)
evolve to the Red Supergiant phase, where they eventually experiment a
blue loop before reaching the Wolf-Rayet stage and/or explode as
a supernova (Langer 1998). For very massive stars (
)
this blue loop occurs at earlier
spectral types, because of a stability limit (de Jager 1991).
In both evolutionary scenarios, the key phenomenon is mass loss, which
generates a circumstellar envelope (CsE).
The distinction between post-AGB stars and supergiants is a difficult
task. Both types of objects are of luminosity class I and they undergo
low-amplitude variations (Kwok 1993). Their circumstellar envelopes can
present large expansion velocities (
15 kms-1).
While so-called "high latitude supergiants'' are now widely believed
to be post-AGB stars (van der Veen et al. 1993), the nature of
low-latitude stars of spectral
types B-G and luminosity class I is more difficult to assess.
This problem is generally addressed through
high-resolution optical spectroscopy, but even then, definite
conclusions are difficult to draw.
HD 179821 (= SAO 124414 = IRAS 19114+0002) is one of these puzzling
objects, being classified either as a post-AGB star
(
3-4
;
e.g. Reddy & Hrivnak 1999) or as a massive supergiant
(
30
;
e.g. Jura & Werner 1999).
We present here an analysis of new millimeter observations of
this source, which clearly favour the post-AGB hypothesis.
A summary of the properties of HD 179821 is given in Sect. 2, with particular emphasis on the controversy about whether it is a post-AGB star or a massive supergiant. A discussion about its distance is also given in Sect. 2. The radio observations are presented and discussed in Sect. 3, in the scope of bringing new constraints on the nature HD 179821.
HD 179821 is of spectral type G5 Ia (Hrivnak et al. 1989) and is located
at a rather low galactic latitude (b II =
). The detection
of OH maser lines implies that it is an oxygen-rich object (Likkel 1989).
It has a double-peaked
spectral energy distribution (SED), with equal amounts of energy from the
photosphere and from the cold dust circumstellar shell (van der Veen et al.
1989). This SED is similar to other post-AGB stars which have experienced
interruption of mass loss (Kwok 1993). This is likely related to the
detached dust shell observed in the mid-infrared (Jura & Werner 1999).
Other remarkable parameters of this object are its expansion and
macroturbulence velocities:
35 kms-1 (Bujarrabal
et al. 1992) and
20 kms-1 (Thévenin
et al. 2000). These values are relatively high compared to similar
objects and, as will be discussed later, affect both the dynamics
and the abundance determinations.
Reddy & Hrivnak (1999) made a detailed analysis of high-resolution optical
spectra of this source. Their LTE analysis gives an effective temperature
(
)
of 6750 K, suggesting a spectral type F, in contradiction
with a previous analysis (Hrivnak et al. 1989).
The high s-process elements abundances support the idea that HD 179821
is a post-AGB object. However, interstellar absorption
components in the Na I doublet suggest a large distance for HD 179821
(
4 kpc), implying a high luminosity (
mag)
and a massive supergiant nature (15-20
).
On the contrary, Thévenin et al. (2000) have based their
composition analysis on medium-resolution spectra, arguing that the strong
macroturbulence in HD 179821 dominates the
spectral line widths and implies strong line blending. They
rejected a high value for
and they adopted a
value of 5660 K, corresponding to a spectral type G0, more consistent
with the usual spectral classification. They did not
find the high s-process elements abundances and they pointed out that moderate
metal deficiency is inconsistent with the massive population I supergiant
hypothesis.
Based on mid-infrared observations, Jura & Werner (1999) studied the
detached dust shell around this star. All their results were interpreted
assuming a 30
supergiant,
as they argued that the high LSR (99 kms-1) and outflow (35 kms-1)
velocities (Zuckerman & Dyck 1986; Bujarrabal et al. 1992) favour this
hypothesis. Nevertheless,
such high expansion velocities have already been observed in well-identified
post-AGB stars (e.g. OH 231.8+4.2 with
= 30 kms-1;
Omont et al. 1993). Another apparently strong argument in favour of a
massive supergiant
concerns the ultraviolet dust opacity, the parameter they denote
.
Based on the model of Jura (1996) and assuming a distance of 1 kpc, they
find
4 105 cm2g-1, well above the values
found for other AGB stars (by a factor
2.7). However, the determination
of
contains some uncertainties. Indeed, according to
Eq. (2) in Jura (1996), one finds
=
,
where
is the average grain cross section and
is the grain
mass, and so
,
with a being the grain size.
Now, only upper limits on the grain size a are given by Jura (1996) for AGB
stars, so that the resulting estimations of
are lower limits.
The estimation for HD 179821 may then be consistent with those for other
low-mass stars. Finally, Jura & Werner (1999) derived a total mass-loss
rate for HD 179821 of
410-4
yr-1 which occured about 1800 yrs
ago, for a distance of 6 kpc and a gas-to-dust ratio of 100. They also found
that this rate was approximately constant with time but probably not
isotropic.
One of the main issues in determining the nature of HD 179821 is the determination of its distance. The kinematic distance of 6 kpc (Zuckerman & Dyck 1986) is widely used to favour the massive star hypothesis. One must keep in mind however, that this value is very uncertain.
First of all, using a simple approximation relation
for the velocity structure of the galactic disk (Lang 1980), the
distance is undetermined for a galactic longitude l II = 35.6
and
95 kms-1. At this longitude, a distance
of 6 kpc is obtained for
= 90 kms-1.
Secondly, as emphasized by Kastner et al. (1993),
this method is valid only if the star lies within the galactic disk. For
a distance of 6 kpc, the height of HD 179821 above the galactic plane
would be 524 pc, which is
relatively high, and well above the scale height for 30
stars
(
90 pc, Miller & Scalo 1979). A height of 90 pc would correspond
to a distance of about 1 kpc, but the resulting low luminosity
(
10
)
is then in contradiction with the hypothesis
of a massive supergiant. Then, the high radial velocity may rather
reflect a past runaway phenomenon (Kastner et al. 1993).
The hypothesis that HD 179821 is a low-mass post-AGB star thus seems to be more robust. We consistently adopt a distance of 1 kpc for HD 179821 in the analysis of the observations we present in the next section, keeping in mind that it may be uncertain by about 50% (Bujarrabal et al. 1992). This results in an uncertainty of about a factor 2 for the derived mass-loss rate, and more generally for all parameters varying as the square of the distance. We will show that, within these uncertainties, this distance is fully consistent with the properties of its circumstellar envelope.
Millimeter observations of molecular lines were reported
by Bujarrabal et al. (1992). They detected the 12CO and 13CO
(1-0) and (2-1) lines, as well as SiO (2-1) and (3-2) lines. They did
not detect the CS(3-2) and the HCN(1-0) lines, which confirms the
O-rich nature of HD 179821. The HCO+(1-0) line was
not detected with a rms of 0.1 K (main beam temperature at the IRAM 30 m
telescope). Bujarrabal et al. (1992) also found clear evidence for departures
from spherical symmetry of the circumstellar envelope. Adopting a
mass-loss rate of 10-3 yr-1 for a distance of 1.5 kpc
(Hrivnak et al. 1989), they found a slight deficiency of 12CO
(12CO/H2 = 10-4), compared to the usual value believed to be
present in O-rich AGB stars.
Omont et al. (1993) have also reported the detection of the
H2S(11,0-10,1) line at a 3
level. Bujarrabal
et al. (1994) detected HNC(1-0) and tentatively SO(65-54).
These two latter molecules may be a sign of an active photochemistry
and/or the presence of shocks in the envelope.
Regarding the recent progress in sensitivity and calibration of
millimeter detectors, we performed in August 1999 new observations at the
IRAM 30 m telescope, on Pico Veleta (near Granada, Spain). Four lines were
observed simultaneously: 12CO(1-0) and (2-1), 13CO(2-1) and
HCO+(1-0). We used SIS receivers at 3 and 1 mm. The half-power beam width is 22
and 10
at 3 and 1 mm respectively. The spectrometers were
256
1 MHz filter banks.
The observations were done by wobbling the secondary mirror to a distance
of 2
from the source. This provides very flat baselines and
thus ensures precise calibration.
The pointing accuracy, checked every hour, was within 3
.
Calibration was achieved with a chopper wheel. The intensities given
hereafter are in units of main beam brightness temperature.
As HD 179821 presents an extended envelope,
we made small maps covering the emission area, with offsets
ranging from
to
,
with step of
in
both right ascension and declination. These maps are thus fully sampled
at 3 mm (12CO(1-0) and HCO+(1-0) lines).
The parameters of the observed lines are given in Table 1
and spectra are displayed in Fig. 1. For the CO lines the given
parameters and the displayed spectra correspond to
the central positions. For the HCO+(1-0) line, both parameters and spectrum
correspond to the average over nine positions, with position offsets ranging
from
to
in both directions. This was done to
increase the signal-to-noise ratio for this very faint line. This allowed
the detection of this line at a 4
level. Although it is weak, this
detection is reliable as it has the same kinematic properties (radial and
expansion velocities) as the strong CO lines.
The emission in all CO lines is resolved. We obtain similar extensions
for 12CO(2-1) and 13CO(2-1), of about 14
,
which implies
a deconvolved radius of 4.9
.
This extension is compatible with
the one already found by Bujarrabal et al. (1992), i.e.
,
as such asymmetry is not detectable
with our sampling.
The 12CO lines are globally parabolic, suggesting optically thick
emission. Such optical thickness is also indicated by the observed
12CO(2-1)/12CO(1-0) line ratio (2.9). Because of
beam dilution effects, the intrinsic value of this ratio is close
to 1. One should note that supergiants generally exhibit larger values
for this ratio (
4), probably because of different excitation
processes around massive stars (Josselin et al. 1998). Furthermore,
all the CO lines are clearly asymmetric, with sharper profiles on the
red edge of the lines. This may be linked to the anisotropy of the mass loss,
pointed out by Jura & Werner (1999). They suggest that the observed
asymmetry in the mid-infrared can be explained by different expansion
velocities towards the north and the south. High resolution maps of the
CO emission would be necessary to see where the relative excess of blue
emission comes from and eventually confirm this explanation.
The 13CO(2-1) line should be optically thinner. This explains the more complex line shape, where features appear, in particular on the red side of the line. This has already been observed by Bujarrabal et al. (1992), who suggest that these features are due to components of receding gas in addition to the "standard'' flow.
line |
![]() |
![]() |
I |
![]() |
rms |
(km s-1) | (K km s-1) | (K) | (K) | ||
12CO(1-0) | 96 | 36 | 64.5 | 1.17 | 0.02 |
12CO(2-1) | 97 | 37 | 172.4 | 3.45 | 0.08 |
13CO(2-1) | 98 | 34 | 53.8 | 1.24 | 0.09 |
HCO+(1-0) | 95 | 35 | 0.3 | 0.01 | 0.003 |
![]() |
Figure 1: Spectra of the observed lines. The vertical dashed line indicates the LSR velocity deduced from the 12CO(2-1) line. The CO lines are zoomed along the velocity range where emission is found in order to emphasize the structure of these lines. The HCO+(1-0) line is shown on a wider velocity range so as to show the reliability of its detection |
Open with DEXTER |
The deconvolved extent of the envelope corresponds to a
linear radius of the molecular envelope,
cm
for a distance of 1 kpc.
For an expansion velocity of
35 kms-1, this implies a
kinematic age
yrs.
After correction for distance, this is half the age obtained from the size of the dust envelope (Kastner & Weintraub 1995). This difference may result from photodissociation of CO by interstellar UV radiation and/or condensation onto grains. Furthermore, as mid-infrared dust emission and millimeter CO lines trace a different epoch of mass loss, this discrepancy between age estimations may be attributed to time variations of the mass-loss rate (Delfosse et al. 1997 and references therein).
For an optically thick CO(1-0) line the mass-loss rate
is estimated from the formula given by Loup et al. (1993):
![]() |
(1) |
![]() |
(2) |
Assuming a stellar luminosity of 104
at 1 kpc (based on
the bolometric magnitude found by integrating the spectral energy
distribution; see Bujarrabal et al. 1992 for a detailed discussion of
the determination of the luminosity)
and the mass-loss rate we propose in the present work, the ratio between
the momentum of the envelope
(
)
and the stellar momentum (
)
is
34.
This value is inconsistent with models of radiation-driven mass loss,
but it is still consistent with the idea of a quasi-explosive ejection of
matter during the post-AGB phase (Bujarrabal 1999).
The observed intensity ratio I(12CO(2-1))/I(13CO(2-1)) is 3.2. However, this value may not give directly the 12C/13C isotopic ratio.
First, we assume that the filling factor is the same for both lines,
observed with the same beam size. It is also reasonable to assume that the
rotational levels are thermalized, since the dipole moment of CO is quite
small (0.1 Debye). Then, the main effect which has to be taken into
account is the 12CO(2-1) line saturation, due to optical thickness.
Other possible effects are selective photodissociation - 13CO
being more easily photodissociated - and chemical fractionation through the
reaction:
![]() |
(3) |
Saturation effects should not be higher than 30% (Knapp & Morris 1985).
We thus obtain an upper limit of 5 for the 12C/13C abundance
ratio. More accurate determination would require radiative transfer
calculations, but also ingredients such as the temperature profile
which is poorly constrained.
This value is remarkably low, but not unusual for a low-mass post-AGB
star. A typical value for RGB stars of initial mass 2-4
is
20. This value can drop down to
10 for a 1
star,
in the case of extra-mixing processes (Charbonnel 1995) and can decrease
during evolution from the RGB to the AGB, even when third dredge-up
occurs (Wasserburg et al. 1995). On the contrary, these extra-mixing processes
such as cool bottom burning should not occur in more massive stars.
Finally, additional processes
should be taken into account to reproduce the low values observed in
the latest stages of stellar evolution (see Palla et al. 2000 for a more
detailed discussion). Indeed, for PNe of initial mass
1-2.5
,
Palla et al. (2000) found an isotopic ratio similar to that of HD 179821.
Interestingly, for such a low initial mass, the star probably did not
experience a 3rd dredge-up (Mowlawi 1999 and references therein),
as precisely found by Thévenin et al. (2000).
Among the molecules detected in the circumstellar envelope of HD 179821, the most remarkable ones are HNC, SO (Bujarrabal et al. 1994) and HCO+ (our present work). Indeed, these molecules may result from an active photochemistry, generated by UV photons emitted by the central star as it warms up, or can be produced in shocks. Shocks may occur around post-AGB stars, in particular in the interacting winds scenario.
HCO+ may be formed through two paths. The first one
invokes the reaction of H3+ with CO, but the survival of the H3+
ion is very short, because of very effective dissociative recombination
(Bachiller et al. 1997). Thus, HCO+ is probably essentially formed
through the reaction
![]() |
(4) |
An ionization front may also be formed by UV radiation from the chromospheres of massive supergiants. But up to now, to our knowledge, HCO+ has never been detected in the envelope of a supergiant. Thus, its detection seems to indicate that the star is of low or intermediate initial mass.
The nature of HD 179821 is subject to debate. It is either a massive supergiant or a rather low mass post-AGB star.
The most widely used argument in favour of the massive supergiant hypothesis
is the kinematic distance, estimated to be about 6 kpc. We showed that
it is very doubtful, as the method used for this determination is not
valid regarding the galactic coordinates of HD 179821 and leads to
a height above the galactic plane (500 pc) too large for
a massive star.
The analysis of our new high-sensitivity radio observations favour the
hypothesis that HD 179821 is a low-mass post-AGB star. First,
the 12C/13C isotopic ratio is rather low,
at most 5. Such a value has been observed towards PPNe and PNe of low
initial mass (2
)
and can be explained thanks to
extra-mixing processes, but it is inconsistent with our current knowledge
of mixing processes in massive stars.
Furthermore, we detect for the first time the
HCO+(1-0) line from HD 179821, which is a signature of
an active photochemistry,
a characteristic of post-AGB stars.
Our conclusions are also fully consistent with
recent determinations of the chemical composition of HD 179821 (Thévenin
et al. 2000).
Additional observations, such as spectrophotometric follow-up and abundance determinations from high-resolution spectroscopy over a wider range of wavelengths than those thus far performed, may bring new independent constraints on the nature of HD 179821.
Acknowledgements
We are grateful to R. Bachiller for providing complementary observations which confirmed the validity of our calibration and for fruitful discussions. We also thank our anonymous referee for comments which greatly improved the presentation of our results. E. J. acknowledges partial support from Spanish grants PB 96-104 and SB 97-22043.