A&A 367, 939-942 (2001)
DOI: 10.1051/0004-6361:20000539
C. R. Cowley1 - S. Hubrig2 - T. A. Ryabchikova4,6 - G. Mathys3 - N. Piskunov5 - P. Mittermayer6
1 - Department of Astronomy, University of Michigan, David Dennison Building, Ann Arbor, Michigan 48109-1090, USA
2 - Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
3 - European Southern Observatory, Casilla 19001, Santiago 19, Chile
4 - Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya 48, 109017 Moscow, Russia
5 - Uppsala Astronomical Observatory, Box 515, 751, 20 Uppsala, Sweden
6 - Institute for Astronomy, University of Vienna, Türkenschanzstrasse 17, 1180 Vienna Austria
Received 5 December 2000 / Accepted 15 December 2000
Abstract
The profiles of H
in a number of cool Ap stars are
anomalous. Broad wings, indicative of temperatures in the
range 7000-8000 K end abruptly in narrow cores. The widths
of these cores are compatible with those of dwarfs with
temperatures of 6000 K or lower. This profile has been known
for Przybylski's star, but it is seen in other cool Ap stars.
The H
profile in several of these stars shows a similar
core-wing anomaly (CWA). In Przybylski's star, the CWA is probably
present at higher Balmer members.
We are unable to account for these profiles within the context
of LTE and normal dwarf atmospheres. We conclude that the
atmospheres of these stars are not "normal''. This is contrary
to a notion that has long been held.
Key words: stars: chemically peculiar - stars: chromospheres - stars: oscillations
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Figure 1:
H![]() |
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Figure 2:
H![]() |
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Both Przybylski and Wegner suggested that these profiles might be understood in terms of an atmosphere that was influenced by severe line blanketing. Within the context of an LTE
calculation, we have been unable to reproduce both the deep, narrow
cores and the wings. Several numerical experiments with blanketed
models were investigated in the preparation of P1. Even if the
boundary temperature were artificially lowered below the values in the
models discussed in that paper, it was not possible to reproduce the
narrow, deep H
core.
At the moment, it is not known whether HD 965 is a rapidly oscillating Ap star (roAp), but other four stars illustrated are known roAp stars.
A CWA is present in H
for some of the stars of Fig. 2, as
shown for one of them in Fig. 3.
The CWA is often less pronounced at H
than H
.
In HD 101065, the anomaly
persists into the higher series members, as was noted by Wegner (1976).
In HD 217522, one can see (Fig. 2)
at H
,
a possible transition case.
The slope of the profile steepens toward the core, beginning
some 3 to 4 angstroms from the line center. This shape is
arguably less noticeable in the other four spectra.
By H
,
the CWA is hardly noticeable in HD 217522.
van't Veer & Megessier (1996) studied H
and H
profiles
of the Sun, Procyon, and the cool Am stars 63 Tau and
UMa (cf. their Fig. 5). More
recently, Gardiner et al. (1999) discussed H
profiles in a
dozen normal stars (including the sun) with effective temperatures
between 5777 K and 9940 K. Their spectra
do not have the sharp break in
slope that can be seen in our Fig. 2.
The recent study of the roAp star HR 3831 (HD 83332) by Baldry & Bedding (2000) may not have had sufficient resolution to reveal a CWA.
We tentatively conclude the
phenomenon is limited to the magnetic sequence of CP stars.
It remains to be seen if it is also limited to the roAp stars.
The best studied cool Ap star that is not a roAp,
is CrB. This star has similar
atmospheric parameters to the roAp star
Equ.
The spectrum of
CrB was obtained at McDonald observatory with a
resolution of 56000. We display it in Fig. 4,
along with a spectrum of
Equ from the same observational run at SAAO
on which the upper two spectra of Fig. 2 were obtained.
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Figure 3:
H![]() ![]() ![]() ![]() ![]() |
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Figure 4:
Observed H![]() ![]() ![]() ![]() ![]() |
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We compare the H
lines for both stars with a theoretical line
profile calculated by spectrum synthesis code SYNTH, which incorporates
the latest version of hydrogen line broadening (Barklem et al. 2001). The comparison is shown in Fig. 4.
Note the following:
We note that a core-wing structure develops in normal dwarfs
with temperatures between 7000 and 8000 K. This is illustrated
in Fig. 5, with the profiles taken from Kurucz (1994).
This structure may account for the reasonable fit shown in
Fig. 4. It is not what we are calling the CWA shown
in Figs. 2 and 3. Those stars are cooler than CrB
and
Equ, and have temperatures closer to
7000 than 8000 K. Their H
profiles have a much
more abrupt change in the slope between
the wing and the core than is seen in normal stars or the
calculations of Fig. 5.
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Figure 5:
Calculated H![]() ![]() |
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Deep cores in an LTE calculation are usually made by a low boundary
temperature. In the case of hydrogen, the high-excitation n = 2level becomes rapidly depopulated as the temperature drops, so that the
cores are relatively insensitive to a lower boundary temperature. We
have attempted arbitrarily adding a cool, dense layer to the top of our
atmospheres. In LTE, low-excitation metal lines become unrealistically
strong well before the H
core becomes as deep as in the
observations.
We have attempted to reproduce the CWA by arbitrary
modifications of the temperature distribution that might be attributed
to convection, or convection in a magnetic, pulsating atmosphere.
These attempts were completely unsuccessful. For the
present, we assume that only a fully non-LTE calculation can
be expected to reproduce the observed profiles.
We have also performed non-LTE calculations using the
MULTI code (Carlsson 1992)
for the first three Balmer lines for two model atmospheres with
and 8000 K. The resulting profiles have slightly (less
than
5%) deeper cores with largest effect in H
,
but we find no
difference in the width of the core. The potential effect of the
partial redistribution during scattering in the line cores
remains to be investigated.
It now seems plain that the atmospheres of magnetic CP stars cannot be
considered normal, even setting aside the well known chemical
inhomogeneities or abundance "patches''.
In addition to the sharp cores of Hand H
,
there is the ionization discrepancy
between the second and
third spectra of the lanthanide rare earths. This problem was
discussed by Ryabchikova and her colleagues (cf. Ryabchikova et al. 2000; Gelbmann et al. 2000), and also in P1. Essentially,
abundances from the third spectra, primarily of Pr III and Nd III are
an order of magnitude greater than those of the second spectra of these
elements.
It is unlikely the ionization anomaly can be due to the neglect of hyperfine structure in Pr III or odd-N isotopes of Nd III, because the lines of these spectra are relatively weak in some of the roAp stars (cf. Ryabchikova et al. 2000, HD 122970 and 10 Aql). Moreover, the same ions can be observed in non-oscillating Ap stars and do not show the same anomaly (Ryabchikova et al. 2001; Weiss et al. 2000). Our partial analysis of HD 965 suggests that the same kind of ionization anomaly exists between Fe I and II. The effective temperature of a model which makes the abundances from Fe I and II lines equal is 8000-9000 K, while the color temperature of the star is in the range 7000-7500 K. A low surface gravity palliates this somewhat, but no realistic gravity will reconcile the ionization and color temperatures.
We are left with distinct indications of two temperatures in models whose structures are quite uncertain. The core depth of the early Balmer lines argues for their formation in a region that covers most of the star. If, indeed, a high layer of gas overlies the photospheres of these stars as in the model by Babel (1992), it could play an important role in the origin of the chemical anomalies of these magnetic Ap stars.
Acknowledgements
CRC thanks many colleagues for helpful conversations regarding HD 965 and the CWA. He thanks Dr. Saul J. Adelman for sending Balmer profiles of several cool Ap stars. Thanks are due to C. van't Veer-Menneret, B. Smalley, and R. Gardiner for commenting on profiles of Am-Fm and normal stars.
Research at the Institute for Astronomy in Vienna received funding from the Austrian Fonds zur Förderung der wissenschaftlichen Forschung (Project S7303-AST).