Issue |
A&A
Volume 504, Number 3, September IV 2009
|
|
---|---|---|
Page(s) | 991 - 1001 | |
Section | Stellar atmospheres | |
DOI | https://doi.org/10.1051/0004-6361/200911949 | |
Published online | 22 July 2009 |
Spectroscopic modeling of oscillating Algol-type stars
I. RZ Cassiopeia![[*]](/icons/foot_motif.png)
A. Tkachenko1 - H. Lehmann1 - D. E. Mkrtichian2
1 - Thüringer Landessternwarte, 07778 Tautenburg,
Germany
2 -
Crimean Astrophysical Observatory, Nauchny, Crimea 98409,
Ukraine
Received 25 February 2009 / Accepted 18 June 2009
Abstract
Aims. Based on time series of high-resolution spectra, we investigate the oEA star (i.e., Algol-type eclipsing binary with an oscillating primary component) RZ Cas to derive precise system and atmospheric parameters and search for phases of rapid mass-transfer and its effects on various system parameters at different epochs of observations.
Methods. We combine a variety of methods including the KOREL program to decompose the components of the spectra and determine the orbital solution, the SynthV program to analyze the disentangled spectra by computing synthetic spectra based on atmosphere models, and the newly developed program Shellspec07_inverse to compute optimized stellar parameters from composite line profiles at all orbital phases.
Results. Based on spectra taken in 2006, the RZ Cas system can be modeled accurately by assuming that only two stars are present. For spectra acquired in 2001, we obtained an improved solution by adding a light attenuating accretion annulus surrounding the primary, but were unable to model remaining structures in the O-C value distribution. The primary of RZ Cas is a normal A-type star that shows no Boo signatures, both components have close to solar abundance. The derived mass of the primary and the separation of the components are slightly smaller than previously assumed. The effective temperature of the primary of 8900 K, is 300 K higher than derived before. The Roche-lobe-filling secondary is assumed to have a large cool spot on its surface pointing towards the primary. We confirm the increase in the orbital period by 2 s between years 2001 and 2006, but not the previously assumed decrease in the orbital radial velocity amplitudes.
Conclusions. With the new Shellspec07_inverse program, we obtained precise stellar parameters of RZ Cas. Results clearly point to the occurrence of a transient phase of rapid mass transfer of RZ Cas in 2001, while in 2006 the system was in a quiet state.
Key words: stars: binaries: eclipsing - stars: variables: general - stars: individual: RZ Cas - stars: oscillations
1 Introduction
RZ Cas (HD 17138, HIP 13133) belongs to the new class of oEA
stars, i.e., Algol-type systems with mass transfer, where the
mass-accreting primary exhibits
Scuti-like oscillations
(Mkrtichian et al. 2002,2004). Investigations of
members of this class are important for at least three reasons.
First, because of the mass transfer in the Algol-type systems, we
can study stellar evolution on a short timescale.
Second, due to the change in the excited oscillation modes during
and after phases of rapid mass transfer, the changing structure of
the outer layers of the gainer star can be investigated by
asteroseismic methods. And third, observations can infer the
basic principles of interaction between the magnetic activity
cycle of the cool secondary, the occurrence of rapid mass transfer
episodes, and the excitation of different non-radial pulsation
modes of the mass-accreting primary. The oEA stars are eclipsing
binaries and basic stellar and system parameters can be directly
obtained by combining photometry and spectroscopy.
During primary eclipse, we also observe the so-called spatial filtration
effect, which means that at these orbital phases the secondary
acts as a spatial filter and produces specific amplitude and phase
changes in brightness and line profiles, depending on the observed
oscillation modes (Gamarova et al. 2003). This effect
can help us to identify the modes in terms of l and m numbers.
RZ Cas (spectral type A3 V+K0 IV) is a short-period (
)
Algol-type system and one of the most well studied oEA
stars. During primary minimum, a partial eclipse is observed
(Narusawa et al. 1994). Olson (1982) and
Varricatt et al. (1998) found evidence of circumstellar
matter surrounding the primary. Single-peaked emission originating
from a structure located between the two stars was detected
by Richards & Albright (1999). These spectra and Doppler
tomography (Richards 2004) indicate that a gas stream was
visible during the observations in 1994. The presence of a gas
stream was also assumed by Rodriguez et al. (2004).
Based on extended photometric observations in 1999, the authors
proposed a hot spot that was present where this stream impacts the
surface of the primary star. The discovery that RZ Cas is also both an X-ray
source (McCluskey & Kondo 1984) and a variable radio
source (Drake et al. 1986) was explained by Umana et al.
(1999) as being caused by the strong coronal activity of
the cool secondary.
RZ Cas was found by Ohshima et al. (1998,2001) to exhibit short-period light variability. They found a dominant oscillation mode of the primary with a frequency of 64.2 c d-1 and this frequency was later confirmed by means of dedicated photometric campaigns by both Mkrtichian et al. (2003) and Rodriguez et al. (2004). From photometric observations acquired until 2000, an apparently mono-periodic behavior with a dominant frequency of 64.2 c d-1 was observed. Lehmann & Mkrtichian (2004, Paper I hereinafter) identified multi-periodic behavior in spectra taken in 2001 with two dominant modes of 56.600 and 64.189 c d-1, both in agreement with the photometric findings by Mkrtichian et al. (2003), who also found that the photometric amplitudes of the principal modes were lower than in 1997-2000. A detailed investigation of the photometric amplitude variability of the principal modes of RZ Cas showed an increase in the amplitude of the 64.189 c d-1 mode in 2001-2006 (Mkrtichian et al. 2007).
In 2006, the star changed its pulsation pattern again: Lehmann & Mkrtichian (2008, Paper II hereinafter) found at least three pulsation frequencies of 64.270, 56.761, and 62.406 c d-1, where the last was observed for the first time. By comparing spectra taken in 2001 and 2006, the authors observed a changing asymmetry in the Rossiter-McLaughlin effect, a much stronger amplitude modulation of the non-radial pulsation modes related to the spatial filtration effect in 2006, and a change in both the orbital period and the pulsation pattern. The authors concluded that RZ Cas has undergone a transient phase of rapid mass transfer in 2001, whereas it was in a quiet state in 2006.
Stellar and system parameters for RZ Cas were derived e.g., by
Maxted et al. (1994) from combined spectroscopy and UBVphotometry (Chambliss 1976), by Varricatt et al.
(1998) from UBV (Chambliss 1976) and J and
K band photometry, by Rodriguez et al. (2004) from
Stroemgren photometry, by Soydugan et al. (2006) from
combined spectroscopy and B and V band photometry, and by us
(Papers I and II) from spectroscopy. From the color indices, the
effective temperature of the primary was derived by Rodriguez et al.
(2004) to be 8600 K, in agreement with Maxted et al.
(1994), whereas Varricatt et al. (1998) adopted a
higher temperature of 8720 K. The mass ratio is given as
q=0.331 by Maxted et al. (1994). Soydugan et al.
(2006) analyzed both the light and radial velocity (RV
hereinafter) curves based on photometric observations from 2002
and spectral data from 2003/2004 by using the Wilson-Devinney program
(Wilson & Devinney 1971; van Hamme & Wilson
2003). For a fixed surface temperature of the primary of
8600 K, the authors derived the temperature of the secondary to
be 4480 K, the mass ratio to be 0.338, the orbital separation
to be 6.87 ,
and the orbital inclination to be 81
98. Varricatt et al. (1998) mentioned that the best-fit model
of the J band light curve is obtained by assuming a dark spot exists on
the secondary.
The present article is our third paper in a series based on a
large number of high-resolution spectra of RZ Cas taken in 2001 and
in 2006. Whereas Paper I described the spectroscopic detection of
Sct-like oscillations in RZ Cas, we investigated in Paper II the differences in the results obtained during the two epochs of
observations such as the different pulsation patterns, the
development of the Rossiter effect, or the different strengths of
the amplitude modulation of the pulsation modes with orbital
phase. We also attempted to model the observed
line profile variations in RZ Cas based on a very simple model with
two spherical stars and Gaussian intrinsic line profiles. Based on
spectra obtained in 2006, the resulting distribution of the O-C
values with orbital phase was very smooth, except for a region
around the secondary minimum where the calculated line profiles were
of greater amplitude than the observed ones. We interpreted this as the
attenuation effect caused by an accretion annulus around the
gainer. However, the model completely failed in the case of the spectra
taken in 2001. The corresponding O-C distribution with
orbital phase showed a complex structure pointing to the necessity
for an improvement in the model by taking typical Algol-type
effects, such as circumprimary matter and a gas stream, into account.
Table 1: Journal of observations.
The aim of the present work is to apply a new computer program called Shellspec07_inverse. This program can model the composite line profiles of eclipsing binary stars in a more robust way by considering intrinsic line profiles computed from atmosphere models as well as the non-sphericity of the Roche lobe filling, cool secondary, and corresponding gravity darkening. By applying Shellspec07_inverse to RZ Cas we attempt to derive precise stellar and system parameters and model effects that we could not explain in Paper II. We start by using the KOREL program (Hadrava 2004b) to compute the disentangled spectra of the components and an orbital solution that includes both stars (Sect. 3). A detailed analysis of the disentangled spectra using synthetic spectra calculated with the SynthV program (Tsymbal 1996) then infers the chemical abundances of the components as well as the starting values of stellar and system parameters (Sect. 4), which are fine-tuned by Shellspec07_inverse (Sect. 5). The model for RZ Cas is described in Sect. 6, and our discussion and conclusions are given in Sects. 7 and 8.
2 Observations and spectra reduction
Data sets containing 951 and 512 spectra of RZ Cas were obtained with the Coude-Echelle-Spectrograph at the 2-m telescope at TLS in 2001 and 2006, respectively. The spectra have a spectral resolution of 33 000 and cover the wavelength range from 4760 Å to 7400 Å. Table 1 gives the journal of observations, where N is the number of spectra obtained in different nights.
Spectrum reduction was completed using standard MIDAS packages, including bias and stray-light subtraction, filtering of cosmic rays, flat fielding, wavelength calibration by a ThAr lamp, and normalization to the local continuum. All spectra were corrected in wavelength for individual instrumental shifts by using a large number of telluric O2 lines.
![]() |
Figure 1: RVs of RZ Cas determined with KOREL, folded with the corresponding periods. |
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3 KOREL analysis
We used KOREL (Hadrava 2004b), a Fourier-transform-based program, that, from a time series of spectra calculates simultaneously the optimized orbital elements and the mean disentangled spectra of the components. The program also considers the variation in the line strengths of the components with orbital phase. From both data sets, we selected all spectra of RZ Cas with S/N>60 and used the wavelength range 4950-5680 Å. The conversion from wavelengths to the RV scale produced 8192 bins of width 5 km s-1, corresponding to a spectral two-pixel resolution of 30 000.
3.1 Orbital solutions
We started by separately analyzing the two data sets from 2001 and 2006, assuming circular orbits and allowing for variable line strengths in the solution. The first two panels in Fig. 1 show the RVs of the primary (black) and the secondary (red) derived from spectra taken in 2001 and 2006 and folded with the corresponding periods. The solid curves show the calculated orbital solutions, zero phase corresponds to the phase of maximum separation. The bottom panel shows the RVs of both components for the data obtained in 2001 (black) and 2006 (red) folded with the period observed in 2006. The Rossiter effect in the RVs of the primary is clearly evident. For both 2001 and 2006, a stronger deviation in the RVs from those expected on the basis of Keplerian motion can be seen in a broad region around secondary minimum. This region is too extended to be caused by the Rossiter effect during secondary eclipse. We discuss in more detail the underlying effect in Sect. 6. Besides this large-scale deviation, the RVs obtained from the spectra taken in 2001 show deviations over short ranges in orbital phase that cannot be found in the data from 2006.
![]() |
Figure 2: Line strength variations of primary (small amplitude) and secondary (large amplitude) calculated with KOREL. |
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Table 2: Orbital elements derived with KOREL.
Figure 2 shows the variation in relative line strengths in both epochs of observation. The increase in the line strength of the secondary during primary eclipse can be seen as it is expected, whereas its decrease during secondary eclipse covers a region in orbital phase that is much broader than the duration of the eclipse and resembles the region of the RV deviations discussed before.
The derived orbital elements are listed in Table 2 where T refers to the time of primary minimum (2 450 000+). The results obtained in Paper II are given for comparison. The version of KOREL that we used did not allow us to determine the errors in the deduced parameters. Thus, we applied a separate program based on the method of differential corrections to the RVs derived with KOREL to estimate the errors in the orbital elements. They are given in Table 2 in parentheses, in units of the last digits.
The values derived for the orbital period in the two epochs of
observation differ significantly, which is similar to the
results of Paper II where we determined the RVs of only the primary
from cross-correlation with a template spectrum. We checked this
additionally by computing the orbital solution with KOREL from the
combined 2001 and 2006 data allowing for a linear trend in orbital
period and RV semi-amplitudes. We inferred a rate of period change of
s y-1 and
km s-1 y-1 for the change in RV
amplitudes (Table 2). We assume that the low accuracy in determining
results from the short time base (7 d) of the
observations in 2001 (see also the large error in P obtained
from the 2001 data) and, in contrast to the results obtained in Paper II,
that the variation in K-values is non-significant. The
difference of 1583 d in the observed epochs suggests that the
total orbital period changed over the 5-yr interval by
(
) s.
Alternatively, the period change can also be determined by using phase shift
information. In this case, the accuracy depends not on the duration of the observation
periods but on the time span
between the two epochs.
In our case, the period change can be determined in this way far more precisely.
If we observe in 2001 an orbital
period of P and in 2006 one of
but fold the RVs measured
from both epochs with
,
we obtain a phase shift of
between the RVs from 2006 and 2001. It follows that
![]() |
(2) |
where




3.2 Spectral disentangling
We used all spectra not acquired during the primary eclipse in 2006 to identify the spectrum of the primary, and all spectra outside secondary eclipse in case of the secondary. In each case, we assigned the orbital elements according to the KOREL solution for that data set. We did not use the spectra from 2001, since they are assumed to be distorted by accretion structures and chromospheric emission from the secondary due to the active phase of RZ Cas in this epoch. For the secondary, we also rejected all spectra with a deviation of the individual RVs from the orbital curve of larger than 7 km s-1. In this way, we obtained 470 measurements for the primary and 247 measurements for the secondary at our disposal.
KOREL yields decomposed spectra normalized to the
common continuum of both stars. Normalization to the individual
continua was completed by using the uvby luminosities derived from
Stroemgren photometry of RZ Cas (Mkrtichian et al.
2009). From an interpolation of the uvby luminosity
ratios (WD solution with hot spot), we derived
![]() |
(3) |
for the wavelength dependence of the ratio of the continua of both stars. Normalization of the disentangled spectra Ri' was achieved by applying
![]() |
(4) |
where



4 Spectrum analysis with SynthV
![]() |
Figure 3: Observed (thick) and calculated (thin) spectra of the primary ( top) and secondary ( bottom) of RZ Cas. |
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Synthetic spectra of the stars were calculated with SynthV
(Tsymbal 1996) and used to derive chemical abundances
of the components and initial values for ,
,
and
for
the stars. Atomic line lists were taken from the VALD database
(Kupka et al. 2000). Model atmospheres for the hot primary
were calculated with LLmodels (Shulyak et al.
2004). For the cool secondary, we used MARCS atmospheres
(Gustafsson et al. 2008) and included an additional
molecular line list taken from Kurucz CDs (Kurucz 1995).
For both primary and secondary,
was fixed to the values
obtained from photometry (see Paper II). We used
,
,
and
elemental abundances as free parameters. In the case of the
primary, we also iterated the value of the microturbulence, whereas
it was impossible to disentangle the values of
and
for
the secondary with its non-spherical configuration and not so well determined
continuum. For the secondary, we therefore fixed
to 2 km s-1. To correct for the
previously mentioned unknown shifts
in a more secure way
than described above, we allowed the shift of the continua of the
disentangled spectra to be an additional free parameter in the
least-squares fit of the calculated by the observed spectra.
Results showed that these additional shifts have always been very
small, so in principle they could be neglected.
Figure 3 shows the observed and calculated spectra. In
the case of the secondary, the fit is not as good as in the case
of the primary because of the more uncertain continuum of this late
type star. Moreover, the normalization of the observed spectrum to
the assumed local continuum is not perfect, even though we
included the full molecular line list and used MARCS atmosphere
models. In addition, the values obtained from the best fit are not
as well constrained because the Fe I lines that dominate
the spectrum have only a low sensitivity to temperature changes in
this temperature range of 4500 to 5000 K. For the primary, we
obtained = (
) km s-1,
= (
) km s-1, and
= (
) K, with
= 4.35 (fixed). Table 3 lists
the differences in the derived abundances from solar, and the mean
error in the measurement is 0.03. The derived abundances are
approximately solar, while Si is underabundant by a factor of 2.5.
For the secondary, we found that
= (
) km s-1 and
= (
) K with
= 3.5 (fixed). In this case, the
derived abundances are close to solar (Table 3), Fe is
underabundant by a factor of 2.6, and Cr by a factor of 4. The mean
error of the measurement is 0.1.
Table 3: Derived abundances of RZ Cas relative to standard solar values.
5 Calculation of the synthetic composite spectrum
Our first attempt to model the composite stellar spectra of spectroscopic eclipsing binaries described in Paper II, was based on simple approximations, such as spherical stars and Gaussian intrinsic line profiles. For the next stage, we decided to use subroutines from the computer program ``Shellspec07'' written by Budaj & Richards (2004) for the computation of synthetic composite line profiles of the stars and the products of Roche overflow (see also Budaj et al. 2005). Hereby we make use of the capabilities of Shellspec07 to compute such spectra for arbitrary orbital phases including eclipse mapping by taking the non-spherical shapes and gravity darkening of the components into account. Moreover, Shellspec07 is well suited to our planned analysis of the distribution of circumbinary matter in different mass-transfer stages since the program can include an optical thin accretion disk and a gas stream and compute the corresponding effects on the resulting spectrum.
The Shellspec07 code is used as a basis for an iterative procedure even though it was not originally meant to solve for individual parameters. Our new program called Shellspec07_inverse solves the non-linear optimization problem by using the Levenberg-Marquardt algorithm. The core of Shellspec07 was implemented as central subroutine for calculating the Roche geometry of the cool secondary, for applying the necessary coordinate transformations in different orbital phases, and for integrating the fluxes from the visible stellar surfaces. For the calculation of intrinsic line profiles we used the SynthV program (Tsymbal 1996). Furthermore, we converted the Shellspec07 program code from Fortran77 to Fortran90 and declared the dynamical arrays to avoid problems with memory allocation.
Shellspec07 calculates the position of the local continuum using a straight line between the outermost points of the considered spectral region. We use SynthV to calculate the line fluxes as well as the continuum fluxes. In this way, the calculation of intensities normalized to the local continuum in Shellspec07_inverse is a trivial task and we do not need any artificial assumption about the continuum location.
5.1 Non-linear optimization of stellar parameters
For solving the inverse problem, i.e., the optimization of stellar parameters
based on the observed spectra, we use the Levenberg-Marquardt algorithm (Marquardt 1963). It determines
the parameters a of a function
y = y(x,a) by minimizing the
merit function
where


Where a'kl represents a Hessian matrix with modified main diagonal





We used a modified, fast version of the Levenberg-Marquardt
algorithm developed by Piskunov & Kochukhov (2002) that
additionally optimizes
within each iteration keeping the
right-hand side of Eq. (6) and the Hessian matrix aklunchanged. We used the described algorithm and modified
routines taken from Shellspec07, and made some additional changes as
described in the next subsections to optimize basic stellar and
orbital parameters, such as the effective temperatures of the binary
components T1 and T2,
for the primary (for the
cool secondary we assume synchronized rotation), RV semi-amplitudes
K1 and K2, the
-velocity of the system, and also the
orbital inclination and the radius of the primary (the secondary
is assumed to fill its Roche lobe). To improve the efficiency of the calculations,
we used all out-of-eclipse phases to optimize the six
first aforementioned parameters, and eclipse phases for the last two.
5.2 Intrinsic line profiles and limb darkening
To compute the intrinsic, rotationally unbroadened, stellar line profiles, we used the program SynthV (Tsymbal 1996) and the atomic line list from the VALD database. Atmosphere models for the more massive, hot primary were computed with the program LLmodels (Shulyak et al. 2004), while we used MARCS atmosphere models for the cool secondary.
Shellspec07 assumes constant intrinsic profiles
and calculates the center-to-limb variation by using a linear limb-darkening law
where the limb darkening coefficient u describes the center to limb variation of the specific intensity. This is a rough approximation since it assumes that the variation over the disk is described by a constant value of u that is independent of line depth. In reality, the limb darkening coefficient strongly varies with line depth and can even reach negative values at the line centers, as shown by Townsend (1997) for the Balmer line cores. Instead of this law, we used SynthV to calculate the profiles for nine different values of

![]() |
Figure 4: Fe I 4957 Å intrinsic line profiles calculated with SynthV at the center of the stellar disk (solid) and at the limb (dashed). Intensity is given in erg cm-2 s-1 Hz-1 rad-1. |
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Figure 5: Limb darkening coefficient for different line depths, derived from the blue (solid curve) and from the red (dotted curve) components of the doublet shown in Fig. 4. |
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5.3 Gravity darkening
Besides the limb darkening of both components, we have to take the gravity
darkening of the Roche-lobe filling secondary into account. It results from the
variation in the effective temperature with local gravity on
the surface of the non-spherical star according to
where







6 Spectroscopic modeling of RZ Cas
6.1 Application to the spectra from 2006
In this phase of the analysis we used the Shellspec07_inverse code described in Sect. 5. According to the conclusion drawn in Paper II that the star was in a quiet state in 2006, we started by analyzing the spectra taken in 2006 using a model that includes only the two stars without considering any effects from circumbinary matter. The deviation of the primary from a spherical shape can be neglected, whereas the secondary fills its Roche lobe. The model assumes a circular orbit and synchronized rotation for the secondary.
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Figure 6:
Time series of observed ( left) and calculated ( center)
Fe I 4957 Å line profiles taken in
2006, folded with the orbital period. The right panel shows the
|
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![]() |
Figure 7:
Left column: surface intensity distributions of the secondary
based on
|
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For the analysis, we averaged the 512 spectra into 100 orbital
phase bins based on the derived orbital period and focused our
investigations on the four most unblended, stronger metal lines:
Fe I 4957, 5056, 5616, and 5625 Å. Figure 6 shows the
phase-binned observed profiles of one of these lines folded with
the orbital period. For each position in phase, the Shellspec07_inverse program
computes a synthetic line profile as shown in the middle panel of
the figure. The Rossiter effect caused by a primary eclipse is clearly
evident in both panels as the S-shaped distortion of the
line profile of the primary. The right panel shows the
two-dimensional distribution of the O-C values normalized to the
individual errors in the measurement (the terms that enter the sum in
Eq. (5) to compute ). This normalized distribution
used to determine the goodness of fit is much smoother than the
O-C distributions shown in Fig. 7. This is because of the
strong variation of the signal-to-noise of the observed profiles
with orbital phase, caused by the different number of averaged
single observations per phase bin and the lower amount of light during
primary eclipse e.g., as seen from the noisy region around phase
0.25 in Fig. 7f. We note that we shifted the primary
eclipse to this phase for clearer visualization.
Figure 7 shows the results obtained by using different
gravity darkening exponents for the cool secondary. We give the surface
intensity distribution in the left row of panels (intensity is in
erg/cm2/s/Hz/rad on a logarithmic scale, distances are in units of
the separation of the components), the O-C line intensity residuals for the
Fe I 4957 Å profiles from 2006 (center row) and from 2001
(right row).
For the gravity darkening exponent of the Roche lobe filling
secondary, we first assumed the value of
as predicted
by theory in the case of a star with a convective envelope.
The assumed model gives a
smooth solution for all orbital phases except for a larger region
around secondary minimum, which appears to be brighter (the
calculated line of the secondary is stronger than the observed
one). This brightening, covering about one fifth of the orbit,
corresponds to an attenuation of the line of the secondary, as
already found for the same region in Paper II and that can also be
seen in the form of a deviation of the RVs from our KOREL solution
(Fig. 1). The
of the Levenberg-Marquardt solution
including all orbital phases is 2.21.
Table 4: Comparison of parameters of the RZ Cas system from literature and obtained with Shellspec07_inverse (see text for a detailed explanation).
In the next step, we tried to model the observed deviations in the
region around secondary minimum assuming that they are caused by
some intrinsic property of the secondary itself. From our point of
view, the most reliable explanation is that the star shows a
different temperature distribution over the surface than we
assumed in our model. Unno et al. (1994) found
that the secondary of RZ Cas can be modeled only by assuming an
unusually large value of the gravity darkening exponent of 0.53 and
inferred that dark spots were present on the front and back sides of
the secondary with respect to the primary. Therefore, we examined
whether an ultra-high value of
could effectively simulate
large, cool spots and improve the
of our spectroscopic
solution. The resulting model (Fig. 7c, d) fits the
observed line profiles in the region around secondary minimum well
but completely fails at phases near primary eclipse, where the
calculated line profiles are much too weak and a dark region in
the O-C frame appears. The resulting
of 2.56 is higher
than the value derived for
= 0.08.
Finally, we divided the stellar surface of the secondary into two
regions by applying
to the hemisphere pointing towards the primary and the
normal value of
to the opposite side
(Fig. 7e). The previously bright region around
secondary minimum was then almost perfectly fitted and no difference
with respect to the first solution (
for the entire
surface) can be seen in the O-C distribution around primary
minimum (Fig. 7f). The resulting
is 1.93. The
remaining, faint structures in the O-C distribution are caused by the
outermost parts of the wings of the lines of the primary where the
observations show a slightly smoother transition than the
calculated profiles whose shapes are dominated by rotational
broadening.
Furthermore, we used Shellspec07_inverse to derive for the primary
km s-1 and
km s-1, and for the secondary
km s-1. The values of the other determined
parameters are listed in the last row of Table 4 and
used in Sect. 7 when compared with previously obtained
values from the literature. The value given there for the radius
of the secondary is in our case derived from the orbital period
and
,
obtained from the analysis of the KOREL decomposed
spectra and represents some mean value of the secondary radius.
Figure 8 shows, for a smaller number of selected phase
bins, a comparison between the observed and calculated line
profiles based on this solution (line profiles
are shifted by a constant value for a clearer visualization).
6.2 Application to the spectra from 2001
![]() |
Figure 8: Comparison between observed (solid) and calculated (dashed) Fe I 4957 Å line profiles. The orbital phase is marked to the right. |
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In a next step, we applied the derived model to the spectra taken in 2001, first without changing any of the parameter values. Figure 7i shows the resulting O-C distribution. We see that the line profile of the primary observed in 2001 is weaker than in 2006, and there is a strong general attenuation along the full orbit.
The residuals represented in Fig. 7ii correspond to the
solution obtained by adding attenuating circumprimary matter of
disk-like structure and both constant temperature and density to the
model. The density of
g cm-3 and
disk temperature of 1050 K were taken from an
unpublished 3D hydrodynamic simulation of mass-transfer in the
RZ Cas system (Mkrtichian et al. 2009) computed with a
program written by Nazarenko (Nazarenko et al. 2001).
The radial extension and thickness of the disk were adjusted
manually. Finally, we assumed a disk with a thickness of
3
(comparable to the diameter of the primary) and a
radial extension from 1.6
(close to the surface of the
primary) to 3
.
This model allows us to adjust the mean
line strength of the primary for all orbital phases in a far more
reliable way, although many structures remain, as can be seen
from Fig. 7ii. Most obvious is the difference in line
strength of the primary between the two half-orbits around first
and second quadrature.
Finally, Fig. 7iii shows the solution obtained by
assuming two different values of the density of the circumprimary
disk of
g cm-3 for the ``bright'' line profiles
of the primary and
g cm-3 for the ``dark'' part
(Mkrtichian et al. 2009). The large-scale differences
in line strength were in this way reduced. However, small-scale,
regional structures of high contrast in the residuals remain.
We confirmed the two suggestions in Paper II that: (i) RZ Cas has undergone a transient phase of rapid mass-transfer; (ii) an accretion annulus around the primary was formed at this epoch. Our model including an attenuating annulus around the gainer significantly improves the solution, compared to that for the model including only the two stars. However, small-scale, regional structures of high contrast in the residuals remain, caused probably by the complex hydrodynamic structure of the circumprimary matter which cannot be modeled with Shellspec07_inverse in its current form.
7 Discussion
By combining several methods based on the KOREL, SynthV and Shellspec07_inverse programs, we have reinvestigated the RZ Cas system based on time series of spectroscopic observations taken in 2001 and 2006. We used the KOREL program mainly to decompose the spectra of the RZ Cas components for spectrum analysis. In this way we also obtained new spectroscopic orbits, based on a different method than those applied in Papers I and II. As is is evident from the type of input data, the method combines the measurement of the RVs of both components (as in Paper I for the centroids of selected lines of both components) with the use of a wider spectral range (Paper II, cross-correlation with a template, but only primary). We now also consider the full range in orbital phase, and KOREL weights the data according to the derived relative line strengths. Our new solution does not reach the formal accuracy of the orbital elements derived from cross-correlation (Paper II). On the other hand, the full information about the composite lines formed in all orbital phases is used. The analysis includes for the first time the secondary based on the spectra from 2006, and allows a comparison of mass ratio and shape of the RV curves derived from the data from 2001 and 2006. These results are compared below with those obtained from Shellspec07_inverse.
Based on the observed phase shift between the two epochs of
observation, we can determine the difference in orbital period very
precisely to () seconds. In Paper II, we also discussed a
decrease in the RV semi-amplitudes by 0.6 km s-1 between the years
2001 and 2006. We showed that a decrease by such an amount cannot
be explained by mass transfer effects and suggested that the
decrease is feigned by distortions in the RVs measured in the
active phase of RZ Cas in 2001. We have now confirmed this assumption,
whether or not the KOREL solution or the Shellspec07_inverse results show
significantly different K values between the 2001 and 2006 data.
The analysis of the decomposed spectra of the components using SynthV resulted in a close fit between the observed spectrum of the primary and the computed synthetic spectrum, whereas the spectrum of the secondary could not be modeled perfectly. One reason for this, besides the lower S/N and the less clearly defined continuum of the fainter, cool-type star is that the SynthV analysis was based on the assumption of a spherical star.
From the spectrum analysis, we did not find any strong metal underabundance of iron peak
elements or
Boo signatures of the primary component as
reported by Narusawa et al. (2006), who found Cr, Ti, Mg and Fe underabundances
of
-0.95, -0.45, -0.55 and -0.63 dex, respectively. Both Cr and Ti have solar
abundance within the errors of measurement. The abundances of Mg
(+0.14 dex) and Fe (-0.16 dex) can also be considered to be close to solar
values. The only remarkable deficiency of -0.39 dex was found
for Si (-0.59 dex by Narusawa). We conclude that the primary
component of RZ Cas is a normal A-type star of nearly solar abundance
Our first application of Shellspec07_inverse to derive stellar and system
parameters of RZ Cas from a non-linear optimization using time
series of line profiles was successful in the case of the
relatively undistorted spectra obtained in the quiet phase of
RZ Cas in 2006. In the following, we compare the results
obtained from different methods. The spectra decomposed with
KOREL represent the mean spectra of the components from all
out-of-eclipse phases. Its analysis using SynthV is based on the
assumption of spherical configurations of both stars. Shellspec07_inverse includes the composite spectra from all orbital phases and
considers Roche geometry and gravity darkening of the secondary.
And it is able to derive the orbital inclination and the radius of
the primary directly from the observed spectra. Since it considers
synchronized rotation and Roche-lobe filling of the secondary, it
will not give values for the radius of the secondary or its ,
however. These values are implicit values depending on the derived
mass ratio, orbital separation, and inclination. A special case are
the effective temperatures of the two stars derived by Shellspec07_inverse. They
were derived from the analysis of only four Fe I lines. In
a narrow sense, they represent only mean line strength scaling
factors for these special lines. Effective temperatures of the
same physical meaning as derived from the decomposed spectra could
be obtained with Shellspec07_inverse only, if we investigated a wider
spectral region as we did in the decomposition. We plan to
explore this much more computer-intensive application using the
least-squares deconvolution (LSD, Donati et al. 1997) of
profiles computed over wide spectral ranges.
The following comparison of derived system parameters is based on
Table 4. It lists the derived system parameters and
compares them with values from literature.
The sources are A) Maxted et al. (1994), B)Varricatt et al. (1998), C) Rodriguez et al. (2004), D)Soydugan et al. (2006), E) this paper, spectra from 2006. Values
that were assumed but not derived by the authors are given in
brackets. Errors in units of the last digit are given in
parentheses. Our value of
for the primary of 8907 K
is only slightly higher than those derived from the analysis of
the disentangled spectrum but more than 300 K higher than the
value of 8600 K derived by both Maxted et al. (1994) and Rodriguez et al. (2004); in contrast, Varricatt et al. (1998) found a value of
8720 K. Based on our model, we can exclude these lower
temperatures from both the Shellspec07_inverse application and from the analysis
of the decomposed spectrum. For the secondary, we obtain
= 4800 K. Although it was derived from only four lines, it
resembles the value derived from the decomposed
spectrum. However, we note that it represents the effective temperature of
the non-spherical secondary only at the pole. The temperature over
most of the surface is lower because of the assumed gravity darkening
(see discussion below).
RV semi-amplitudes or K-values derived from RVs measured from
line centroids are based on a model that does not include any
non-sphericity effects or effects that occur during the eclipses
(Rossiter effect). KOREL derives the orbital solution from RVs
weighted by the derived line strengths and suppresses in this way
the influence of the Rossiter effect on the orbital solution, but
does not also consider non-sphericity effects. Shellspec07_inverse derives the
RV semi-amplitudes or K-values by considering the effects of
non-sphericity on line shapes as well as the line asymmetries
during the eclipses (eclipse mapping). Thus, it should provide the
most reliable mass ratio of the stars that we determined to be
.
This value is clearly higher than the values
between 0.331 and 0.338 determined by previous authors. The
derived mass of the secondary agrees within the errors of
measurement with the values derived by other authors except for
Soydugan et al. (2006). Thus, the higher value of the
mass ratio is caused by the lower value of the mass of the primary
of (
)
that we obtained, and the
smaller separation of (
)
.
The derived
radius of the primary of (
)
and the
orbital inclination of (
)
agree well with the
values derived by Soydugan et al. (2006).
Comparing the rotational period of the primary of (
) d
derived from the radius and
with the orbital one, we find, to
within the errors of measurement, that the primary rotates
synchronously.
If we assume that the surface intensity distribution of the
secondary is only influenced by limb and gravity darkening, the
most accurate solution is found by applying a gravity darkening exponent of
0.5 to the hemisphere of the secondary pointing towards the
primary, and the usual value of 0.08 to the opposite hemisphere. Of course, we
are aware that we derived such an exotic value of because we tried to model some inhomogeneous surface intensity
distribution that may arise e.g., from the presence of spots by
applying a law that describes a completely different physical
effect. The improved modeling of the observations provided by this
high value of
suggests the presence of a large dark spot
that dominates the surface region pointing to the primary and that
may have a smooth transition to the other parts of the surface. If
the reflection effect is taken into account, we expect to measure an even
higher value of the gravity darkening exponent since this effect
would brighten in particular the surface covered by the dark spot.
These findings partly in agree with those by Unno et al. (1994), where authors found a gravity darkening
exponent of
.
They concluded that spots on the front
and back sides of the surface of the secondary (pointing towards
and away from the primary) are formed as the result of
mass-outflow. However, we found no evidence of such a cool dark spot on
the back side of the secondary as also suggested by Varricatt et al. (1998).
The application of the model derived from the spectra taken in
2006 to those from 2001 showed a strong attenuation of the line of
the primary, inferring that there is dense circumprimary
matter and that a transient phase of rapid
mass-transfer occurred shortly before the observing period in 2001 as
already suggested in Paper II. The attempt to model this attenuation
by introducing optically thin circumprimary matter of disk-like
structure in Shellspec07 provided a significantly improved
solution. The
of the solution decreases in this
case and decreases even more if we assume different densities of
the disk in two different regions of the orbit. Complex structures
in the O-C distribution however remain.
8 Conclusions
The new Shellspec07_inverse program has been successfully applied to time series of spectra of the oscillating Algol-type star RZ Cas obtained during its quiet state in 2006. The derived mass of the primary and the separation of the components are slightly smaller than previously obtained from photometry and spectroscopy, whereas the temperatures of both components are slightly higher. All other system parameters agree with at least one of the previous determinations. Shellspec07_inverse takes the full spectroscopic information from line profiles in all orbital phases including eclipse mapping as well as the non-sphericity of the Roche lobe filling secondary and an improved modeling of gravity and limb darkening into account. For these reasons and the large number of spectra analyzed, we believe that the stellar and system parameters of RZ Cas derived in this work are the most precise spectroscopically derived so far.
We have detected a distortion over a broad range of phases around secondary minimum that we interpret as the effect of a dark spot on the surface of the secondary pointing towards the primary. This effect can be seen in the RVs obtained with KOREL as well as in the corresponding line strengths and residuals of the Shellspec07_inverse solution, assuming normal gravity darkening. Since the surface intensity distribution of the secondary can be modeled well by assuming a very high value of the gravity darkening exponent, a very large dark spot must be present that has a smooth transition to the surrounding stellar atmosphere.
We also determined the abundances of the components and conclude
that both components have approximately solar abundance with a
slight underabundance of Si for the primary and of both Cr and Ni for
the secondary. From the orbital solutions, we derive a precise
value of the increase in the orbital period of () s
between the two epochs of observations in 2001 and 2006, in
agreement with the photometric findings (for a detailed discussion
of period changes see Paper II).
The application of Shellspec07_inverse to the spectra obtained in 2001 shows that the system cannot be described by including only the two stars into the model. The situation is improved by adding an attenuating accretion annulus surrounding the primary but complex structures in the 2D O-C distribution remain. This result confirms our conclusion drawn in Paper II that the star had undergone a transient episode of rapid mass transfer shortly before the observations in 2001. It also shows, however, that a very detailed map of the circumbinary gas distribution is needed to ensure more robust modeling.
In the future, we plan to work with Shellspec07_inverse also on LSD profiles
calculated from wider spectral regions so that the results for
atmospheric parameters such as
are more
representative. We also plan to develop a more detailed model of
the structure of circumbinary matter during active phases, and to
apply the program to other Algol-type stars.
Acknowledgements
We would like to thank Jan Budaj for providing us with the latest version of the Shellspec07 program and for his help in software usage. We are grateful to Vadim Tsymbal for providing us with the SynthV code and to Oleg Khochukov for the modified version of the Levenberg-Marquardt algorithm as well as for their steady help and useful comments. We want to thank the referee, Mercedes Richards, for her substantial comments that helped us to improve the article considerably.
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Footnotes
- ... Cassiopeia
- Based on observations with the 2-m Alfred Jensch telescope at the Thüringer Landessternwarte (TLS) Tautenburg.
All Tables
Table 1: Journal of observations.
Table 2: Orbital elements derived with KOREL.
Table 3: Derived abundances of RZ Cas relative to standard solar values.
Table 4: Comparison of parameters of the RZ Cas system from literature and obtained with Shellspec07_inverse (see text for a detailed explanation).
All Figures
![]() |
Figure 1: RVs of RZ Cas determined with KOREL, folded with the corresponding periods. |
Open with DEXTER | |
In the text |
![]() |
Figure 2: Line strength variations of primary (small amplitude) and secondary (large amplitude) calculated with KOREL. |
Open with DEXTER | |
In the text |
![]() |
Figure 3: Observed (thick) and calculated (thin) spectra of the primary ( top) and secondary ( bottom) of RZ Cas. |
Open with DEXTER | |
In the text |
![]() |
Figure 4: Fe I 4957 Å intrinsic line profiles calculated with SynthV at the center of the stellar disk (solid) and at the limb (dashed). Intensity is given in erg cm-2 s-1 Hz-1 rad-1. |
Open with DEXTER | |
In the text |
![]() |
Figure 5: Limb darkening coefficient for different line depths, derived from the blue (solid curve) and from the red (dotted curve) components of the doublet shown in Fig. 4. |
Open with DEXTER | |
In the text |
![]() |
Figure 6:
Time series of observed ( left) and calculated ( center)
Fe I 4957 Å line profiles taken in
2006, folded with the orbital period. The right panel shows the
|
Open with DEXTER | |
In the text |
![]() |
Figure 7:
Left column: surface intensity distributions of the secondary
based on
|
Open with DEXTER | |
In the text |
![]() |
Figure 8: Comparison between observed (solid) and calculated (dashed) Fe I 4957 Å line profiles. The orbital phase is marked to the right. |
Open with DEXTER | |
In the text |
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