A&A 474, 307-314 (2007)
DOI: 10.1051/0004-6361:20078082
P. Quinet1,2 - C. Argante1 - V. Fivet1 - C. Terranova1 - A. V. Yushchenko3,4 - É. Biémont1,2
1 - Astrophysique et Spectroscopie, Université de Mons-Hainaut,
7000 Mons, Belgium
2 - IPNAS (Bât. B15), Université de Liège, Sart Tilman,
4000 Liège, Belgium
3 - Astrophysical Research Center for the Structure and
Evolution of the Cosmos, Sejong University, Seoul 143-747, South Korea
4 -
Astronomical Observatory, Odessa National University, Park Shevchenko, Odessa 65014, Ukraine
Received 14 June 2007 / Accepted 13 August 2007
Abstract
Radiative data for transitions of astrophysical interest
in radioactive elements Ra I, Ra II, Ac I and Ac II have been
computed using a semi-empirical relativistic Hartree-Fock approach
including core polarization effects. Most of the oscillator
strengths reported in the present paper are new. A possible
detection of radium (Ra II) and actinium (Ac II) in the spectrum
of the stars HD 101065 and HR 465 is examined and discussed.
Key words: atomic data - stars: chemically peculiar
In astrophysics, the first detection of short-lived radioactive elements in stellar atmospheres was made by Merrill (1952) who identified Tc I lines in the spectra of S-type stars. A few years later, Przybylski (1961) discovered a star (HD 101065) with properties that placed it far outside of the known limits of the stellar peculiarities. More precisely, Cowley et al. (2000) performed abundance determination of this star for 54 elements and found that lanthanides were overabundant by 4-5 dex. The overabundance of thorium and uranium was also reported in the same paper while Cowley (2003) and Cowley et al. (2004) confirmed with a high degree of confidence the presence of lines of radioactive technetium and promethium. In addition, Gopka et al. (2004) presented the results on new identification of the lines of all radioactive elements with atomic numbers from Z=84to Z=99, except for Z=85 (At) and Z=87 (Fr). The presence of these heavy short-lived radioactive elements in Przybylski's star is enigmatic. Cowley et al. (2004) proposed that some unrecognized processes, such as flare activities, were taking place in the atmosphere of the star. On the other hand, Gopka et al. (2004) suggested that the presence of elements with Z<92 is due to the natural radioactive decay of thorium and uranium in the upper atmosphere while the existence of elements with Z>92 could be due to neutron capture in the stratified layers of the atmosphere with large overabundance of thorium and uranium. A discussion about possible explanation for the existence of short-lived radioactive elements in stellar atmospheres can also be found in Goriely & Arnould (2001), Gopka et al. (2006) and Yushchenko et al. (2006, 2007). In a recent paper, Goriely (2007) has stressed the importance of spallation nucleosynthesis compared to diffusion processes as a possible explanation of the peculiar abundances spectroscopically determined at the surface of HD 101065. Although it remains difficult to disentangle the effect of both processes theoretically, this conclusion does not necessarily reduce the role of the diffusion processes which have proven to be of first importance to understand the atmosphere of CP stars. As stressed by Goriely (2007), "the contribution of the nuclear process would be greatly strengthened if spectroscopic observation could confirm the presence of short-lived radioelements at the surface of CP stars and, if confirmed, hopefully in a close future provide abundance determination for these clear tracers of nuclear activity''. Unfortunately, for most of the 72 lines of radioactive elements listed by Gopka et al. (2004) in the spectrum of HD 101065, oscillator strengths are not known. As a first attempt to fill in this gap, we report in the present paper atomic structure calculations for transitions of astrophysical interest in Ra I, Ra II (Z=88), Ac I and Ac II (Z=89).
According to the NIST compilation (Moore 1971), very few energy levels are known in Ra I. In fact, 13 even- and 28 odd-parity levels have been identified by Rasmussen (1934a) with the revisions suggested by Russel (1934) on the basis of the comparison of Ra I with the analogous Be I, Mg I, Ca I, Sr I and Ba I spectra. These levels were established from 69 classified lines from 2955.65 Å to 9932.21 Å and interpreted as belonging to the 7s2, 7s7p, 7s6d, 7s8s, 6d7p, 7s8p, 7p2, 7s7d, 7s9s, 7s5f, 7s6f, 7s7f and 7s8f configurations. In Ra II, Rasmussen (1933, 1934b) classified 64 lines between 1888.7 Å and 9453.57 Å, from a hollow-cathode source and stressed the similarity of this spectrum with the Ba II one. This gave rise to well-established ns (n=7-11), np (n=7-9), nd (n=6-12), nf (n=5-7) and ng (n=5-11) Rydberg series.
For Ac I and Ac II, the energy levels reported in the NIST compilation (Moore 1971) are based on the observation of the emission spectrum of actinium due to Meggers et al. (1957) who analyzed arc and hollow-cathode spectrograms made at the Argonne National Laboratory by Fred et al. (1955). In these spectra, 87 Ac I lines, with wavelengths ranging from 2968.82 Å to 7866.10 Å, were classified as combinations among 6 even and 34 odd energy levels while 226 Ac II lines, with wavelelengths from 2261.75 Å to 7886.82 Å, were classified as combinations of 27 even and 38 odd levels. These levels were interpreted as belonging to the 6d7s2, 6d27s, 7s27p, 6d7s7p, 6d27p configurations (Ac I) and to the 7s2, 7s6d, 6d2, 7s7p, 6d7p, 7s5f, 7s8s and 5f7p configurations (Ac II).
In a more recent compilation on actinide elements due to Blaise &
Wyart (1992), the spectrum of Ac I was not reanalyzed. For Ac II,
however, the energy levels from the early analysis by Meggers et al. (1957) were reinvestigated by the parametric Slater-Condon
method which led to a few changes in the theoretical assignments.
The studied configurations were 7s2 + 6d2 + 6d7s + 5f2 +
5f7p and 5f6d + 5f7s + 6d7p + 7s7p, respectively. This led to
reject the two levels 5f7p 3G5 and 6d5f 3H
reported in the NIST compilation (Moore 1971) and to find four new
even levels between 56 491 and 64 285 cm-1 from the 80 lines
which remained unclassified after the analysis by Meggers et al. (1957).
Available transition rates and lifetime values in neutral and singly ionized radium and actinium are very sparse.
In the case of Ra I, oscillator strengths were calculated for the
7s2-7s7p transitions using the relativistic pseudo-potential
approach (Hafner & Schwarz 1978), the multiconfiguration
Dirac-Fock method (Bruneau 1984) and the relativistic local spin
density functional (Sen & Puri 1989a). More recently, the
multiconfiguration Dirac-Hartree-Fock model was employed to
compute oscillator strengths for the 7s2 1S0-7s7p
1P
electric dipole and the 7s2 1S0-7s6d
3D2 electric quadrupole transitions (Bieron et al. 2004) while relativistic Hartree-Fock method (Dzuba et al. 2000) and many-body perturbation theory (Dzuba & Ginges 2006)
were used to compute transition probabilities for lines connecting
the low-lying states belonging to the 7s2, 7s7p and 7s6d
configurations. The lifetime of the 7s7p 3P
level
was experimentally determined by Scielzo et al. (2006) by
measuring the exponential decay of fluorescence after illuminating
a thermal atomic beam with pulses of laser light.
For Ra II, the only attempts to obtain radiative data are due to Lindgård & Nielsen (1977), who considered a simple Coulomb approximation and to Sen & Puri (1989b), Glushkov (1991) and Glushkov et al. (1996), who used essentially model-potential approaches. In one recent work (Biémont et al. 2004), oscillator strengths were computed for the first ions along the francium isoelectronic sequence, including Ra II, using the pseudo-relativistic Hartree-Fock and the fully relativistic Dirac-Fock methods.
In the case of actinium, the only available results were obtained by Sen & Puri (1989a) who used the relativistic spin density functional approach to compute oscillator strengths for the 7s2-7s7p transition array in Ac II. However, to our knowledge, no transition rates were published for Ac I.
For heavy neutral and lowly ionized atoms such as those considered
in the present work, accurate calculations of atomic structure
should allow for both intravalence and core-valence correlation.
In addition relativistic effects must normally play an important
role. A method which has appeared as a suitable compromise between
a gratifying accuracy of the results (tested by comparison with
accurate laser lifetime measurements), the moderate complexity of
the codes used and the ability to obtain many new results in a
limited period of time, is the relativistic Hartree-Fock (HFR)
technique as described by Cowan (1981) but modified by us for the
inclusion of core-polarization (CPOL) effects. In this approach
(HFR+CPOL), most of the intravalence correlation is represented
within a configuration interaction scheme while core-valence
correlation is described by a core-polarization model potential
and a correction to the dipole operator depending upon two
parameters, i.e. the dipole polarizability of the ionic core,
,
and the cut-off radius,
(for details see e.g.
Quinet et al. 1999). Although based on the Schrödinger
equation, this method takes the most important relativistic
effects, such as the mass-velocity contribution and the Darwin
correction, into account.
We have introduced in the model explicit intravalence interactions
between the configurations 7s2 + 7s8s + 7s9s + 7s6d + 7s7d +
7s8d + 7s9d + 6d8s + 6d9s + 6d7d + 6d8d + 6d9d + 6d2 + 7p2 +
7d2 + 5f2 + 5f7p + 5f8p + 5f9p + 5f6f + 5f7f + 5f8f + 5f9f
(for the even parity) and 7s7p + 7s8p + 7s9p + 7s5f + 7s6f + 7s7f
+ 7s8f + 7s9f + 6d7p + 6d8p + 6d9p + 7p7d + 7p8d + 7p9d + 7p8s +
7p9s + 6d5f + 6d6f + 6d7f + 6d8f + 6d9f + 5f7d + 5f8d + 5f9d +
5f8s + 5f9s (for the odd parity). Core-polarization effects were
included using the dipole polarizability,
,
equal to
18.62 a03, as tabulated by Fraga et al. (1976) for the
ionic core Ra2+ while the cut-off radius,
,
was chosen
to be equal to 2.07 a0 which corresponds to the expectation
value of r for the outermost core orbital (6p6) as calculated
with Cowan's codes. The HFR+CPOL method was combined with a
least-squares optimization routine minimizing the discrepancies
between calculated and experimental energy levels compiled by
Moore (1971). More precisely, for the even parity, the average
energies,
,
the exchange Slater integrals, G2(s,d), and
the spin-orbit parameters,
,
corresponding to the 7s6d
and 7s7d configurations were adjusted while only the average
energies of 7s2, 7s8s, 7s9s and 6d2 were optimized. It
should be noted here that the average energy parameter of 6d2was fitted instead of the one corresponding to 7p2 because the
three energy levels (at 31248.84, 32214.84 and 32941.13 cm-1)
identified in the NIST compilation (Moore 1971) as belonging to
7p2 were predicted, in our calculations, as mainly belonging to
6d2, the 7p2 configuration appearing a few thousands of cm-1 above (around 37 000 cm-1). This prediction is
confirmed when comparing Ra I with the analogous Ba I spectrum in
which the 6p2 configuration is situated
10 000 cm-1above 5d2. For the odd parity, all the radial parameters
(
,
Fk, Gk,
)
corresponding to the
7s7p, 7s8p and 6d7p configurations were adjusted while only
average energies were fitted for 7s5f, 7s6f, 7s7f and 7s8f
configurations. The standard deviations, as defined by Cowan
(1981) were found to be equal to 194 cm-1 for the even parity
(13 levels and 10 variable parameters) and 260 cm-1 for the
odd parity (28 levels and 16 adjustable parameters).
The physical HFR+CPOL model used here was exactly the same as the
one described in our previous paper related to Fr-like ions Ra II,
Ac III, Th IV and U VI (Biémont et al. 2004). In this
model, all the ns, np, nd, nf, ng and nh
configurations up to n=12 were included while core-polarization
corrections were considered with
a03 and
a0. The semi-empirical process was then performed
using all the experimental energy levels taken from the NIST
compilation (Moore 1971). More precisely, the average energies
(
)
and the spin-orbit parameters (
)
were adjusted
to reproduce exactly the doublet energy levels belonging to the ns
(n=7-12), np (n=7-9), nd (n=6-12), nf (n=5-7) and
ng (n=5-11) configurations.
For this atom, intravalence correlation was considered by means of
the inclusion of the following configurations in the HFR model :
6d7s2 + 6d27s + 6d28s + 6d3 + 6d27d + 7s27d +
7s28s + 6d7p2 + 7s7p2 + 7p27d + 7p28s + 5f6d7p +
5f6d8p + 5f7s7p + 5f7s8p + 5f7p7d + 5f7p8s + 6d7s7d + 6d7s8s +
6d7p8p + 6d7d8s + 7s7p8p + 7s7d8s (even parity) and 7s27p +
7s28p + 7p3 + 5f6d2 + 6d27p + 6d28p + 5f7s2 +
5f7p2 + 7p28p + 5f6d7s + 5f6d8s + 5f6d7d + 5f7s7d + 5f7s8s +
5f7p8p + 6d7s7p + 6d7s8p + 6d7p7d + 6d7p8s + 6d7d8p + 6d8s8p +
7s7p7d + 7s7p8s + 7s7d8p + 7s8s8p (odd parity). Core-polarization
effects were considered with the dipole polarizability tabulated
by Fraga et al. (1976) for the Ac3+ ion, i.e.
a03, and the cut-off radius taken from
Cowan's code as the expectation value of r for the 6p6orbital in actinium, i.e.
a0. For the even parity,
the six experimental energy levels belonging to the 6d7s2 2D
and 6d2(3F)7s 4F multiplets tabulated by Blaise & Wyart
(1992) allowed us to adjust the average energies and spin-orbit
parameters corresponding to these configurations. Unfortunately,
for the odd parity, despite the fact that all but two energy
levels of the 6d7s7p configuration are reported in Blaise &
Wyart's compilation, we were unable to obtain a reasonable fit by
adjusting the corresponding radial parameters. More precisely,
when adjusting all the radial parameters (average energy,
spin-orbit parameters and electrostatic integrals) corresponding
to 6d7s7p, the average deviation between calculated and
experimental energy levels was found to be equal to 853 cm-1,
this value being only reduced to 826 cm-1 when introducing
the "illegal-k'' effective operators (Cowan 1981). This could be
due to the fact that one or several experimental energies are
affected by large uncertainties. Another reason could be that the
6d27p configuration, which is expected to interact strongly
with some 6d7s7p levels, is unsufficiently known to allow a
simultaneous adjustment of all parameters, including configuration
interaction integrals, corresponding to both configurations. Other
low-lying configurations such as 7s27p, 7s28p, 5f7s2could also play a role. Although included in our physical model,
the fact that these latter configurations are completely unknown
experimentally could explain the poor quality of the fitting
process. Consequently, in the present work, only average energies
were adjusted for 6d7s7p and 6d27p configurations. However, in
order to optimize the final results, the theoretical transition
energies were replaced by experimental values when computing the
oscillator strengths.
The Ac II ion belongs to the radium isoelectronic sequence.
Consequently, the same set of interacting configurations as the
one used for Ra I was explicitly included in the physical model.
For the core-polarization parameters, we used the same values as
for Ac I, i.e.
a03 and
a0. The semi-empirical procedure was applied to the 7s2,
7s8s, 7s6d, 6d2 even configurations and to the 7s7p, 7s5f,
6d7p, 6d5f odd configurations for which all the corresponding
radial parameters were adjusted using the experimental level
energies tabulated by Blaise & Wyart (1992). In addition, in
order to reduce as much as possible the discrepancies between
calculated and experimental energy levels, an effective
interaction parameter
(Trees 1951a,b; Racah 1952)
associated to the 6d2 configuration was considered in the
fitting process while the generalized Slater integrals Rkcorresponding to the configuration interactions between 6d7p and
7s5f, on the one hand, and between 6d7p and 7s7p, on the other
hand, were also adjusted. It is worth noting that the new
spectroscopic designations of some levels proposed by Blaise &
Wyart (1992) compared to the previous analysis due to Meggers et al. (1957) were confirmed in the present work. Although some
levels belonging to 5f7p are known experimentally, we preferred
not to include those levels in the fitting procedure because,
according to our calculations, they are situated in a region (from
55 000 to
65 000 cm-1) where many levels of unknown
configurations such as 7p2, 6d8s, 6d7d and 7s7d appear. The
standard deviations were found to be equal to 179 cm-1 for
the even parity (15 levels and 10 variable parameters) and 280 cm-1 for the odd parity (38 levels and 22 adjustable parameters).
Table 5: Oscillator strengths for transitions in Ra I.
Table 6: Oscillator strengths for transitions in Ra II.
The computed energies, Landé g-factors and eigenvector compositions as obtained in the present work for low-lying levels in Ra I, Ra II, Ac I and Ac II are reported in Tables 1-4 together with the available experimental data.
Oscillator strengths obtained in the present work are reported in Tables 5-8 for selected transitions of Ra I, Ra II, Ac I and Ac II, respectively. For most of these transitions, listed as strong lines by Sansonetti & Martin (2005), radiative data are reported for the first time (see also http://physics.nist.gov/PhysRevData/Handbook/Tables/radiumtable2.htm and http://physics.nist.gov/PhysRevData/Handbook/Tables/actiniumtable2.htm).
Table 7: Oscillator strengths for transitions in Ac I.
Table 8: Oscillator strengths for transitions in Ac II.
For Ra I, a comparison between radiative lifetimes deduced from
our calculations and available results is shown in Table 9. With
the exception of the 6d7s 1D2 level (
E = 17 081.45 cm-1), for
which our computed transition probabilities are affected by large
cancellation effects, a good agreement (5-20%) is observed
between the values calculated in the present work and the recent
ones obtained by Dzuba & Ginges (2006) using the many-body
perturbation theory. For the 7s7p 3P
level, our
calculated lifetime (
ns) is
30% shorter than
the experimental measurement due to Scielzo et al. (2006).
In order to see whether this difference could be due to an
underestimation of core-polarization effects included in our
theoretical model, we have performed semi-empirical HFR
calculations including explicitly core-valence correlations by
means of additional configurations with one hole in the 6s or 6p
subshell, instead of considering the core-polarization potential.
More precisely, the following configurations were added to the
ones considered in the physical model presented in Sect. 3.1.:
6s26p57p3 + 6s26p56d27p + 6s26p57s27p +
6s26p56d7s7p + 6s6p66d3 + 6s6p66d27s +
6s6p66d7s2 + 6s6p66d7p2 + 6s6p67s7p2 (even
parity) and 6s26p56d3 + 6s26p56d27s +
6s26p56d7s2 + 6s26p56d7p2 + 6s26p57s7p2+ 6s6p67p3 + 6s6p66d27p + 6s6p67s27p +
6s6p66d7s7p (odd parity). Using this model, the calculated
lifetime for the 7s7p 3P
level was found to be
equal to 250 ns, i.e.
10% shorter than our HFR+CPOL
calculation and
40% shorter than the measurement due to
Scielzo et al. (2006). This indicates that core-polarization
corrections were not underestimated in our HFR+CPOL model, having
in mind that HFR calculations without core-polarization gave a
lifetime value of 215 ns. It was also verified that, for the levels
at 13 715.85, 13 999.38, 16 688.54, 17 081.45 and 20 715.71 cm-1, the
magnetic dipole (M1) and electric quadrupole (E2) contributions were
negligible.
Table 9: Comparison of lifetimes of low-lying states of Ra I.
For Ra II, a comparison between our oscillator strengths and
previous results was already presented in our recent paper related
to Fr-like ions (Biémont et al. 2004). In that paper, we
pointed out that our multiplet f-values were 25% lower than the
results obtained for the 7s-7p transition by Sen & Puri (1989b)
using the quasi-relativistic local spin density functional
approach. However, the results obtained in our work were
considered to be more reliable than those published by Sen & Puri
in view of the excellent agreement observed between the accurate
lifetimes measured by Zhao et al. (1997) and Simsarian et al. (1998) for the levels 7p1/2 and 7p3/2 in the
isoelectronic francium atom and our calculations performed using
exactly the same model as the one used for Ra II (Biémont et al. 1998). It was also shown in Biémont et al. (2004)
that our results were in reasonable agreement with those of
Lindgård & Nielsen (1977), Glushkov (1991) and Glushkov et al. (1996), using the Coulomb approximation and a model
potential method, respectively, for the 7s-7p, 7p-8s, 8s-8p,
6d-7p, 7p-7d and 7d-8p transition arrays in singly ionized
radium. Very recently, the 7s-7p electric dipole and 7s-6d electric quadrupole
matrix elements in Ra+ were evaluated by Safronova (2007) using a relativistic coupled-cluster method in which single, double and partial triple
excitations of Dirac-Fock wavefunctions were included to all orders of
perturbation theory. The theoretical lifetimes taken from this study
for 7p1/2 (
ns), 7p3/2 (
ns),
6d3/2 (
s) and 6d5/2 (
s) are in
excellent agreement (within a few percents) with the values deduced from the
present work, i.e.
ns, 4.97 ns, 0.611 s and 0.316 s,
respectively.
In the case of actinium, the only available result for comparison
is the one published by Sen & Puri (1989a) for the 7s21S0-7s7p 1P
transition in Ac II. The
oscillator strength computed by these authors (log gf =
0.45) is considerably larger than the result obtained in the
present work (log
gf = -0.21). This is probably due to the fact
that the quite simple model used by Sen & Puri (1989a)
underestimated the strong mixing between the 7s7p
1P
and 6d7p 3D
states. In fact, for
the level at 33 388.61 cm-1, classified as 7s7p
1P
in the NIST tables (Moore 1971), our
calculations gave a mixing of 61% 6d7p 3D
+ 23%
7s7p 1P
,
in very good agreement with the
composition (60% + 28%) obtained by Blaise & Wyart (1992) using
the parametric Slater-Condon method. Moreover, it is interesting
to note that, when performing a very simple HFR calculation,
including only 7s2 and 7s7p configurations, we could obtain an
oscillator strength (
)
in good agreement with the
one published by Sen & Puri (1989a).
The calculation of ionization equilibrium in stellar atmospheres using Saha equation requires the evaluation of the partition functions for neutral and ionized species. The values computed in the present work for radium and actinium are given in Table 10 for temperatures from 3000 to 14 000 K. These results were obtained, for each element, using the available experimental levels completed with all the calculated values deduced from the theoretical models described in Sect. 3. This corresponds to total numbers of levels equal to 539, 78, 1722 and 539 for Ra I, Ra II, Ac I and Ac II, respectively. In order to estimate the detrimental effect of missing experimental levels on the partition functions, the latter were also computed using only the available experimental energies. When doing so, it was found that the partition functions reported in Table 10 were almost unaffected for T = 3000 K while they were decreased by a factor of 2.06, 1.04, 2.73 and 1.06 for T = 14 000 K in the case of Ra I, Ra II, Ac I and Ac II, respectively.
Table 10: Partition functions in Ra I, Ra II, Ac I and Ac II.
As pointed out by Cowley et al. (2004), Gopka et al. (2004) and Bidelman (2005), the lines of radioactive elements can be identified in the spectra of Przybylski's star (HD 101065) and of HR 465. Yushchenko et al. (2007) tried to estimate the abundances of actinides, forcing all oscillator strengths to zero. Using the new atomic data obtained in the present work for radium and actinium, we investigated the astrophysical spectra of these two stars.
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Figure 1: Three Ra II lines in the spectrum of Przybylski's star. Tentative identifications have also been performed for neighbouring lines but they are very uncertain in some cases. The x- and y-axis correspond to wavelengths (in Å) and intensities (in arbitrary units), respectively. |
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Some of the wavelengths reported in Tables 5-8 being shorter than
3000 Å, we first used observed IUE spectra from INES archive,
namely LWR06999HL for the Przybylski's star and LWP14571HL,
LWP14572HL, LWR03984HS, LWR03987HS, LWR07217HL, LWR14522HL,
LWR14526HL for HR 465. The spectral resolution (R) of IUE
spectra is about 0.1 Å while the signal to noise ratio
(S/N) is in the range extending from 10 up to 30. Observed
spectrum of Przybylski's star at longer wavelengths (from 3040 to
10 350 Å) was taken from VLT archives (Bagnulo et al. 2002). This spectrum is characterized by a resolution of 80 000 and
a S/N ratio greater than 300. For HR 465, we used two spectra
for wavelengths longer than 3000 Å. The first one (
=
4000-6800 Å,
R = 40 000, S/N = 70-100), registered in
1996 with the 1.93 meter telescope of Haute-Provence Observatory
(France), was extracted from the archives of this observatory
(Prugniel & Soubiran 2001). The second spectrum (
=
3780-9500 Å,
R = 80 000, S/N > 100) was observed in 2004
with the 1.8 m telescope of Bohuynsan Observatory (Korea). It
should be mentioned that, due to the strong variability of
spectral lines in HR 465 with a period of 22-24 years (Preston &
Wolff 1970), the first spectrum shows enhanced chromium lines
while the second one shows enhanced lanthanide lines.
Both HD 101065 and HR 465 stars have very complicated spectra with a significant part of spectral lines being unidentified. Yushchenko et al. (2007) showed that strong stratification of chemical elements could exist in the atmosphere of Przybylski's star but, unfortunately, there is presently no accurate atmospheric model susceptible to describe the observed spectrum of this star correctly. Consequently, we restrict ourselves, in the present paper, to a short discussion of possible identifications of some lines of radium and actinium in the spectra of these two stars.
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Figure 2: Same as Fig. 1 for the HR 465 star. |
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Figure 3: The six spectral regions around possible Ac II lines in the spectrum of Pzrybylski's star. The x- and y-axis correspond to wavelengths (in Å) and intensities (in arbitrary units), respectively. |
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In fact only three Ra II lines could be used to estimate the upper
limit of radium abundance in the atmospheres of the investigated
stars if dedicated stellar models were available. These lines,
located at 3814.42, 4682.28 and 8019.70 Å, are shown in Figs. 1 and 2 for HD 101065 and HR 465 stars, respectively. For the
first line (
Å), the observed wavelength is
3814.40 Å in Przybylski's star and 3814.39 Å in HR 465. This
line is free of strong blending. For the line at 4682.28 Å, we
found no counterparts in the observed spectra. The Y II line at
4682.324 Å is the strongest blending line in the spectra of
both stars while the Os I line at 4682.06 Å should influence
the spectrum of Przybylski's star only. Ra II line at 8019.70 Å
is too weak and could not be identified. The spectral region
around this wavelength could be used for determining an upper
limit to the stellar content of radium.
The search for actinium lines in the HR 465 spectrum was not
successful. For most of the lines, the appearance of the observed
spectrum can be explained by lines of other elements. In contrast,
actinium lines could possibly be present in the spectrum of
Przybylski's star. Figure 3 shows the observed spectra of HD 101065 and identifications of the strongest lines. For the Ac II
line at 3043.30 Å, the observed wavelength is 3043.01 Å. Some
blends could be due to Ce II (3043.268) and Tb III
(
3043.324) lines but the influence of these lines is not
expected to be important.
For the line at 3069.36 Å, the
observed wavelength at 3069.345 Å is free from strong blending
but the Ce II line at 3069.318 Å should however be taken into
account. The Ac II line at 4061.60 Å, observed at 4061.556 Å in the HD 101065 spectrum, could be blended with Nb I
(
4061.539) and Zr I (
4061.515) lines. The line
at 4168.40 Å, observed at 4168.436 Å, is one of the best lines
for which actinium can make the largest input to the absorption
feature, the lines of other elements being weak except the Co I
contribution at
4068.443. Finally, the Ac II lines at
5758.97 and 5910.85 Å (observed at 5758.97 and 5910.865 Å)
are not expected to be affected by strong blends and the
identification of these lines as due to actinium is plausible
according to the available linelists.
Oscillator strengths have been calculated for strong lines in neutral and singly ionized radium (Ra I-II) and actinium (Ac I-II). For most of the transitions considered in the present work, f-values are reported for the first time. These new results are intended to provide astrophysicists with some of the data they need for quantitative investigations of stellar spectra where such radiaoactive elements are expected to be observed. The two cases of HD 101065 and HR 465 are considered. A close examination of the spectra indicates that some absorption features observed in the spectra of these stars could possibly be due to Ra II and Ac II. A more quantitative analysis however is awaiting the availability of accurate models describing the atmospheres of these stars.
Acknowledgements
P.Q. and E.B. are respectively Research Associate and Research Director of the Belgian Fund for Scientific Research (F.N.R.S.). V.F. has a fellowship of the F.R.I.A. Financial support from these organizations is acknowledged. A.Y. was supported by the Astrophysical Research Center for the Structure and Evolution of the Cosmos (ARCSEC) of the Korea Science and Engineering Foundation (KOSEF) through the Science Research Center (SRC) program. We thank Dr. M.S. Safronova for sending us some results in advance of publication.
Table 1: Comparison between experimental and calculated energy levels in Ra I.
Table 2:
Experimental energy levels and calculated Landé g-factors in Ra II. For this ion, the
differences
cm-1 and the eigenvector purities are equal to 100% for all the levels (see the text).
Table 3: Comparison between experimental and calculated energy levels in Ac I.
Table 4: Comparison between experimental and calculated energy levels in Ac II.