Issue |
A&A
Volume 520, September-October 2010
|
|
---|---|---|
Article Number | A103 | |
Number of page(s) | 17 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/200913726 | |
Published online | 08 October 2010 |
Spectroscopic analysis of the B/Be visual
binary HR 1847
,![[*]](/icons/foot_motif.png)
J. Kubát1 - S. M. Saad2 - A. Kawka1 - M. I. Nouh2 - L. Iliev3 - K. Uytterhoeven4 - D. Korcáková1 - P. Hadrava5 - P. Skoda1 - V. Votruba1,6 - M. Dovciak5 - M. Slechta1
1 - Astronomický ústav, Akademie ved Ceské republiky, 251 65 Ondrejov,
Czech Republic
2 - National Research Institute of Astronomy and Geophysics, 11421
Helwan, Cairo, Egypt
3 - Institute of Astronomy, Bulgarian Academy of Sciences, 72
Tsarigradsko Shossee Blvd., 1784 Sofia, Bulgaria
4 - Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, CEA, IRFU,
SAp, Centre de Saclay, 91191 Gif-sur-Yvette, France
5 - Astronomický ústav, Akademie ved Ceské republiky, Bocní II 1401,
141 31 Praha 4, Czech Republic
6 - Ústav teoretické fyziky a astrofyziky PrF MU, Kotlárská 2, 611 37
Brno, Czech Republic
Received 24 November 2009 / Accepted 22 May 2010
Abstract
We studied both components of a slightly overlooked visual
binary HR 1847 spectroscopically to determine its
basic physical and orbital parameters. Basic stellar parameters were
determined by comparing synthetic spectra to the observed echelle
spectra, which cover both the optical and near-IR regions. New
observations of this system used the Ondrejov and Rozhen 2-m telescopes
and their coudé spectrographs. Radial velocities from individual
spectra were measured and then analysed with the code FOTEL
to determine orbital parameters. The spectroscopic orbit of
HR 1847A is presented for the first time. It is a
single-lined spectroscopic binary with a B-type primary,
a period of 719.79 days, and a highly eccentric orbit
with e=0.7. We confirmed that HR 1847B is
a Be star. Its
emission
significantly decreased from 2003 to 2008. Both components
have a spectral type B7-8 and luminosity class IV-V.
Key words: binaries: general - stars: emission-line, Be - stars: individual: HR 1847
1 Introduction
HR 1847 (HD 36408, BD +16794,
HIP 25950, ADS 4131) is a bright visual binary
consisting of two B type stars. Throughout this paper, the component at
,
will
be denoted as HR 1847A
(or component A) and the one at
,
as
HR 1847B (or component B). The
first observations of this binary, which were obtained on
31 December 1782, were reported by William Herschel
(see Herschel 1785,
star III.93). He observed this binary again on
21 January 1800 (see Herschel
1821, star 124).
Athough this visual binary consists of two bright stars and Plaskett (1919) recommended further observations, it was not studied much during the last century. Since HR 1847 is both an X-ray source (Berghöfer et al. 1996) and an IRAS source (Coté & Waters 1987), and considering its brightness, lack of observations, and sometimes confusing catalogue information, it has become quite an interesting object for more detailed study.
2 Summary of known properties of HR 1847
In this section we summarize the information currently available for both components of HR 1847, which is scattered throughout the astronomical literature, online catalogues, and databases.
2.1 Multiplicity
2.1.1 Angular separation
Angular separation
and relative position
of the components of HR 1847 have already been measured by
Friedrich Georg Wilhelm Struve (1837,
star No. 730) as an average of
4 measurements obtained in 1829 and 1832 (
,
).
Later measurements resulted in
,
(Cannon 1912b),
,
(Russell & Moore 1929),
,
(Perryman et al. 1997,
from HIPPARCOS),
,
(Fabricius et al. 2002,
from the Tycho catalogue),
,
(Mason et al. 2004, from
speckle interferometry). The angular separation, as reported
by Lindroos (1983) and Abt & Cardona (1984)
is
.
2.1.2 Radial velocity variations
The first radial velocity measurements for both components were reported by Plaskett & Young (1919) and they showed variability. Plaskett et al. (1920) suggested that both components are spectroscopic binaries. Frost et al. (1926) designated HR 1847A (No. 126 in his Table II) as a spectroscopic binary with an unknown orbit using only one spectrum secured at the Dominion Astrophysical Observatory (DAO) in 1919 by Otto Struve. Component A was also reported to be a spectroscopic binary by Gahm et al. (1983) and Abt et al. (2002). However, no attempt has been made to determine the orbital parameters until now.
2.2 Distance
The HIPPARCOS parallax of HR 1847 is 2.92
1.57 mas (Perryman
et al. 1997), which corresponds to a distance of
342
184 pc, but the large error reduces the reliability of this
distance estimate. However, the new edition of the HIPPARCOS catalogue (van Leeuwen 2007) gives a
parallax value of 1.09
2.04 mas, which is unable to provide any information about the
distance owing to the very uncertain parallax. Individual parallax
measurements of the A and B components are
not available.
2.3 Magnitudes and photometry
Table 1:
HIPPARCOS and
photometry of HR 1847.
The first reliable magnitude values (VA=6.07, VB=6.44) were published by Cannon (1912b). She also gives the combined AB magnitude as 5.49. Maybe that only the combined magnitude value was given in her earlier spectral classification (Cannon 1912a) and in the HD catalogue (Cannon & Pickering 1918) caused its being incorrectly but often quoted as the magnitude of the A component until now. A similar value is also listed in the Bright Star Catalogue (V=5.46, Hoffleit & Jaschek 1991).
The photometry of HR 1847 was measured by several
authors always during observing runs devoted to large sample of stars. Eggen (1977) measured
photometry of early type stars and
derived values VA=6.1
and VB=6.5.
Lindroos (1983) measured
photometry
of visual binaries including HR 1847.
He derived corresponding V magnitudes of
both components from
the y filter values as VA=6.091
0.019 and VB=6.510
0.023.
observations
of visual binaries at Mount Maidanak were performed by Shatskii (1998), and he obtained VA=6.09
0.02 and VB=6.51
0.02. The EXPORT
photometry
(observed by the Nordic Optical Telescope, Oudmaijer
et al. 2001) gave values VA=6.09
0.10 and
VB=6.49
0.07. Recent determinations of magnitudes were derived from HIPPARCOS
photometry (see Perryman
et al. 1997). With the HIPPARCOS VT
and BT magnitudes,
Kharchenko (2001) derived the
magnitudes VA=6.056
0.008 and VB=6.451
0.004, which do not differ too much from the first values of Cannon.
A more complete list of photometric magnitudes of both
components of HR 1847 is given
in Table 1.
2.4 Polarization
Oudmaijer et al. (2001)
found the value of V band polarization PV
= 0.0063
0.0004 for the A component, and PV
= 0.0063
0.0002 for the B component.
2.5 Spectral types and luminosity classes
The early classification of both components was ``egregie alba'' (very white) by Struve (1837). Later, (Cannon 1912b) classified both stars as B9.
Using his own observations in the period from April 1954 to March 1955 at the Yerkes Observatory, Osawa (1959) determined the spectral type of component A as B7IV and of component B as B8IV. From his own observations with the Perkins telescope, Slettebak (1963) determined spectral types B7III for component A and B7IV for component B. Cowley et al. (1969) determined spectral types B8III and B8V for components A and B, respectively, using spectra from MacDonald and Yerkes Observatories. Levato (1975) observed both components at Cerro Tololo Inter-American Observatory and obtained spectral type B7III for component A and B8IV for B. Finally, Mora et al. (2001) changed the Bright Star Catalogue classification of HR 1847A from B7IIIe to B5V.
2.5.1 Emission
Andrews (1968) found that
component B shows
emission using
photometry,
which was later spectroscopically confirmed by Wackerling
(1970). The emission sign, which appeared at the spectral
type of component A in both the Bright Star Catalogue and the
Simbad database, is incorrect, as
emission was never reported for HR 1847A.
2.6 Rotation
Rotational velocities of both components were first determined by Slettebak (1963). The projected
rotational velocity of component A was measured as ,
while component B was found to be rotating rapidly,
.
Levato (1975) determined
and
.
Abt et al. (2002)
refined the values of the rotational velocities to
and
using coudé spectra obtained at the Kitt Peak 0.9-m telescope.
2.7 Variability
Slightly different values of magnitude obtained at different times using different instruments, which are listed in the Sect. 2.3, cannot be considered as firm proof of variability. The only available homogeneous set of observations was obtained by the HIPPARCOS satellite. Using HIPPARCOS photometry, Percy et al. (2004) determined the characteristic time scale of variability for HR 1847 as 0.9 days. They conclude that it is a classical Be star, but it is not clear which component they are refering to, since both components A and B have HIPPARCOS photometry available. In addition, data for both components also include several values that correspond to the combined magnitude of both components. Since it is not clear that they excluded the apparently wrong values (those corresponding to combined A+B magnitude), their result is questionable. We performed an independent search for variability and could not confirm the variability time scale found by Percy et al. (2004).
2.8 X-rays
HR 1847 has also been identified as an X-ray source by ROSAT (Berghöfer et al. 1996) with
an X-ray luminosity
(in the paper version). In the online version of the
same catalogue (their Table 2),
this value is slightly different,
.
Both corresponding values of
(or -6.79 in the online version) correspond to a typical
relation
for B-type X-ray emitters (cf. Berghöfer
et al. 1997). It is, of course,
a question of which star of the pair is the X-ray source,
if not both. The position of the ROSAT
source 1RXS J053214.9+170319 suggests it is more
probably coincident with the star
TYC 1301-1942-1 = HR 1847B (Flesch & Hardcastle 2004);
however, the positional error is
(Voges et al. 2000),
so HR 1847A also lies within the error circle.
2.9 IR excess
In their study of IR excess of 101 Be stars Coté & Waters (1987) found IRAS magnitudes [12]=4.95, [25]=2.22, [60]=-0.92, which places HR 1847 in the [12]-[25]/[12]-[60] colour-colour diagram far away from the region where almost all Be stars are located. Coté & Waters suggest there is a reflection nebula close to HR 1847. Whitelock et al. (1989) associate HR 1847 with the IRAS SSSC source X0501+589. Magnier et al. (1999) suggest that HR 1847 is a good candidate for a Herbig Ae/Be star with a very large or a very cool circumstellar disk, but Iwata et al. (1999) did not find any CO emission for this star.
Again, it is not clear which star has IR excess, but most
likely it is component B, which was found to be
a Be star. There is also a small possibility that
both stars are Be stars, with component A not in
emission at that moment. Further observations may shed a light
on it. Coté & Waters
(1987) attributed the spectral type B7IIIe to
HR 1847, which corresponds to component B, and ,
which corresponds to component A.
2.10 Cluster membership
Although HR 1847 is located in the same region as the open
cluster Collinder 65 (A component is #771,
B component #772, according to the WEBDA database),
its membership is improbable mainly because to the different
proper motion (Kharchenko
et al. 2004).
3 Observations and data reduction
The data available for this study consist of several data sets of
electronic spectra mostly centred on the
region:
4 Component A
- 68 spectra in the spectral range 6250-6770 Å
obtained with a CCD SITe ST-005 800
2000 pix camera attached to the coudé spectrograph of the 2 m-telescope in Ondrejov (Czech Republic). The spectra were obtained between 18 October 2003 and 25 February 2008. Spectra were reduced using IRAF
.
- One spectrum obtained on 22 March 2003 with the red
(5850-8450 Å) and blue (3800-5650 Å) channels of the
fiber-fed echelle spectrograph HEROS (resolving
power
20 000, for its brief description see Kaufer 1998). The spectrograph was attached to the Cassegrain focus of the 2 m-telescope at the Ondrejov Observatory. All the basic data reduction processing was done using the HEROS pipeline written by Otmar Stahl and Andreas Kaufer as an extension of the basic MIDAS echelle context (see Stahl et al. 1995, also Skoda & Slechta 2002).
- 14 spectra obtained in the spectral range
(6510-6608 Å) at Rozhen Observatory (Bulgaria) using the
coudé-spectrograph of the 2 m RCC telescope. The CCD
camera Photometrics AT200 with an SITe SI003AB 1024
1024 CCD chip (24
24
m pixel size) was used in the f/9.5 camera of the spectrograph to provide spectra with a spectral resolution of 36 000 in the H
region. Spectra were obtained between 24 October 2004 and 30 August 2007 and reduced with the MIDAS package.
- One spectrum in the spectral range 6290-6745 Å obtained at Observatório do Pico dos Dias (OPD, Brasil) and published by Vieiria et al. (2004). For details and information about the reduction process, see the reference above.
5 Component B
spectra came from the same instruments as mentioned in the preceding part describing spectra of component A.- 38 spectra obtained using the Ondrejov coudé spectrograph between 17 October 2003 and 22 March 2008.
- One HEROS spectrum obtained at the Ondrejov Observatory, one night after the HR 1847A spectrum, on 23 March 2003.
- Three spectra between 28 August 2007 and 30 August 2007 obtained at the Rozhen Observatory.
3.1 Radial velocity measurements
Radial velocities were measured using the code SPEFO,
which was developed by the late Dr. Jirí Horn (see also Skoda 1996). The FITS
files obtained from IRAF and MIDAS
were transformed to the SPEFO format, and then
the radial velocities (RVs) were
obtained interactively by means of the best match of the line profile
with its mirror.
The RVs were obtained for hydrogen ,
He I 6678 Å, Si II 6347 Å
and 6371 Å lines. RV data for individual components
are described later in this paper
in Sects. 4.2
and 5.1.
4 Component A
4.1 The effective temperature and gravity
The spectral region observed by HEROS covered the range 3800-8620 Å (see Figs. A.1 and A.2) and was used to determine the spectroscopic effective temperature and surface gravity. The line spectrum of the star is quite poor. Balmer lines up to H10 and some infrared lines are seen. No emission is present in the Balmer lines and in the lines of other metal ions.
The effective temperature and surface gravity were determined
by comparing the observed spectra to model spectra. We used the ATLAS9
LTE line blanketed model atmospheres, which were calculated by Kurucz (1993)
assuming solar metallicity and microturbulent velocity 2
.
All synthetic spectra were convolved (using the code ROTIN3
by I. Hubeny) with the Gaussian function having FWHM = 0.25
to reduce the resolution of the synthetic spectra to the observed
resolution. We used a
-fitting
routine to compare the whole observed spectra with the synthetic ones,
and we obtained a best fit of
and
0.5.
Following the temperature scale of Theodossiou
& Danezis (1991), these values correspond to spectral
type B7-B8, and from the value of the surface gravity, we
estimate the luminosity class as IV-V. The quoted error bars
correspond to the adopted steps of our model grid, which are
in temperature and 0.5 in
.
Using the code ROTIN3, we calculated a
grid of rotationally broadened spectra for
with a step of 5
.
Then we applied the
fitting
routine again to determine the best rotational velocity for this star.
To do this, we used the spectral line Mg II 4481 Å
(recommended by Gray 1976, as a
line free of pressure broadening) in
the fitting process. We determined the projected rotational velocity of
HR 1847A as
,
which differs by 5
from the value of Abt et al.
(2002). The error of our value of the rotational velocity was
calculated employing a 1-
error algorithm of Zhang et al. (1986).
4.2 Radial velocities
![]() |
Figure 1:
The radial velocity variations for hydrogen |
Open with DEXTER |
Tables A.1
and A.2
display the line radial velocity measurements that were derived using
the methods described in Sect. 3.1.
Columns 1-3 represent the file identification, HJD, and the
heliocentric RVs, respectively. Column 4 lists the
RV measurements for the line.
Columns 5-7 list the RVs measurements for He I 6678 Å,
Si II 6347 Å, and Si II 6371 Å
(which are weak) absorption
lines, respectively. The measured RVs were shifted to the zero-point
using a set of sharp telluric absorption lines by means of the
technique described in Horn
et al. (1996).
The RVs of HR 1847A vary between 8
to 27
with a mean velocity around 13
.
Figure 1
displays the measured RVs for hydrogen
and He I 6678 Å as a
function of time. The plots indicate that our RV measurement
started with one value just before the RV maximum, then after
the maximum, a clear decrease in the RV values is
recorded until the RV values reach their minimum around
HJD 2 453 620 with RV values of
9-10
.
Then they quickly reached the next maximum value of 27
around HJD 2 453 670. Although only two
cycles are covered by our observations, fortunately we successfully
recorded two epochs of rapid rise to the maximum, which happened during
a very short time (nearly 35 days) of the long cycle.
Rozhen observations confirmed the present distribution of RVs.
Such a relatively short event could easily be missed.
The RV measurements that were obtained with different lines in
the region
show the same distribution with time, and only a small difference in
the maximum height can be recognized, as illustrated for the
He I 6678 Å line (lower
panel of Fig. 1).
4.3 Period determination
![]() |
Figure 2:
Upper panel: power spectrum of measured RVs
of |
Open with DEXTER |
![]() |
Figure 3:
Phase diagram of measured RVs for |
Open with DEXTER |
One of the most fundamental parameters of binary systems is the orbital period. The present RVs span an interval of 1801 days. From the inspection of the time plot one can conclude that
- 1.
- the present RV measurements of
and of some other metalic lines show clear evidence of long-term cyclic variability; and
- 2.
- the relatively large scatter between individual measurements on successive nights indicates that shorter period variability could be present in the data distribution.
For PERIOD, starting values for the
frequencies need to be given, and frequency values are improved within
the limits given by the window function. We used this program to search
for periodicities in both
and He I 6678 Å RV data
sets in the range between 1 to 1000 days,
with an expected frequency resolution of
.
The upper panel of Fig. 2
displays the periodogram of the detected frequencies in this period
range.
It shows three candidate frequencies (indicated by arrows in
the upper panel of Fig. 2),
namely 0.0069
,
0.0014
,
and 0.1077
.
The frequency 0.0069
has power 61, and is dominant. The middle panel of
Fig. 2
shows the spectral window. In the lower panel of Fig. 2 we show the power
spectrum of the residual periodogram prewhitened for 0.0014
(using PERIOD), which clearly shows the
disappearance of all peaks related
to all three candidate frequencies.
Using the PDM technique we searched for periodicity in
intervals 1-10 days, 1-100 days, and
1-1000 days. The results are summarized in Table 2 and agree with the
ones
obtained with PERIOD. Figure 3 illustrates the
phase diagrams of measured RVs
for the line
folded with the
,
and
frequencies.
Table 2: Candidate frequencies resulting from the PDM period search.
Although the frequency 0.0069
has the highest power (cf. Fig. 2 and Table 2), we suspect that
this frequency is not a real one. First, the historical
observations of Plaskett &
Young (1919) are out of phase by about half of the period
(open squares in the middle panel of Fig. 3). Second, the
corresponding RV curve predicts a maximum of RVs near
HJD 2 453 350, which was not confirmed by
our observations. Values around
appear instead of maximum ones. In addition, the interval of
145 days (or approximately five months) roughly
corresponds to the gap between the end of one season in
March/April and the next start of observations in August/September.
Third, the candidate frequency 0.0069
is almost exactly equal to 5
0.0014
.
The relative scatter of individual RV values folded with the
0.1077
frequency is quite large. Following these arguments, we propose the
frequency at 0.0014
as the dominant frequency.
4.4 Orbital solution
Table 3: Orbital elements of HR 1847A with FOTEL.
The variability of the radial velocities with frequency
0.0014
can most likely be explained by binarity, and it supports the earlier
idea of Plaskett & Young (1919)
that the star is a
spectroscopic binary.
Starting from the frequency 0.0014
,
we performed 4 different orbital solutions using the program FOTEL
developed by Hadrava
(1990,2004).
For the solutions denoted as I, II, and III (see
Table 3),
the orbital elements were derived for
radial velocity
variations with data observed from different sites. Solution I
is only performed with Ondrejov data, Solution II is obtained
using
measurements
from both Ondrejov and Rozhen
observations, Solution III is obtained using all of the
available data, namely Ondrejov and Rozhen observations, one spectrum
from OPD, and including the historical measurements.
Solution IV was obtained using radial velocities of all
available spectral lines in the
region
(
,
He I 6678 Å, Si II 6347 Å,
and Si II 6371 Å).
In our calculations we allowed the period, eccentricity,
periastron longitude, and semiamplitude to converge. For each data set FOTEL
also allows individual -velocities
to be determined.
Figure 4
illustrates the FOTEL Solution III with
its
residuals.
We searched for additional periodicities in the residuals but did not
find any significant periods.
We adopt the Solution III (
,
e=0.70
0.02) as an orbital solution of HR 1847A.
![]() |
Figure 4:
Upper panel: radial velocity curve of the
primary component corresponding to the FOTEL
orbital solution III (
|
Open with DEXTER |
5 Component B
![]() |
Figure 5:
The evolution of the |
Open with DEXTER |
The B component is a Be star with a relatively weak emission in
and almost negligible one in
.
Since 2003, the weak emission in
further weakened, indicating an approaching end of the
Be phase. No time scale may be given for this
apparently long-term variability, since only 4 years of
observations are available. Long term variability (strengthening and
weakening of emission) is typical of Be stars on time scales
from years to tens of years (for a review see Hubert
2007). For example,
Dra has quite a
well-established long term time
scale, and its most recent determination is 22.11 years (see Kubát et al. 2010, and
references therein). The
profiles obtained by our observations are plotted in Fig. 5. We fitted the
spectrum of component B using the same methods as for
component A.
We found
,
,
and
.
5.1 Radial velocities
Owing to the high rotational broadening of lines in the
component B spectrum, the helium and silicon lines,
which were used for RV measurement
of component A, are too shallow in
component B, and therefore unusable for
RV measurement. Consequently, we measured the RVs of
component B only from the line.
RVs were measured with the profile inversion technique.
However, the rapid rotation of the component B and
relatively low S/N made it impossibile to arrive at precise
RV values.
Cross-correlation techniques, such as least-square
deconvolution (LSD, Donati et al.
1997) would not improve the RV accuracy as too few line
profiles are available in our spectra. Also, the bisector
method does not give more accurate results because of the limited
quality and not high enough S/N of our spectra.
The
line in the B component is characterized by a double-peak emission with
peaks of equal strength. We measured the RVs of three different
features at the
line,
namely of the line wings, of the emission part, and of the
central absorption. The results are listed in Tables A.3 and A.4 and plotted
in Fig. 6.
Although the RVs are evidently variable, a period search did not give any reasonable result. That is why we cannot make any conclusions about the possible binarity of HR 1847B until a more complete set of more accurate data has been obtained.
6 The possible A+B system
There is a question as to whether the components of this visual pair are physically bound. However, there is not enough data to help to resolve this question. The history of all relative position measurements of HR 1847 in the sky (see Sect. 2.1.1) do not allow any conclusion about their relative motion. Slightly different values can be attributed to errors in individual measurements.
Unfortunately, only a common parallax measurement from HIPPARCOS is available. Since individual measurements are missing, we cannot easily say whether the A and B components are at the same distance. However, study of visual binaries by Shatskii (1998) suggests that HR 1847 could be a physical system (with a period shorter than 1 Myr), since both components have similar proper motion and corresponding photometric parallaxes, which agree with the hypothetical parallax.
![]() |
Figure 6:
Time evolution of the |
Open with DEXTER |
Table 4: Summary of parameters of both components of HR 1847.
In case the visual components of HR 1847 are
physically bound, their similar spectral type suggests that they are of
similar age. Then there is the question of why one of these stars
developed an
envelope that causes emission
and the other does not. The emission could not be caused by mutual
interaction between components A and B, simply
because the distance between the components
is too large. A different mechanism for the origin of the
Be phenomenon in HR 1847B has to be found (see, e.g.,
the review by Porter &
Rivinius 2003). The emission in the component B is
most probably connected with its rapid rotation. Projected rotational
velocity of component A is lower, and this star also
has no emission. On the other hand, since the inclination
angles are unknown, we can not exclude the possibility that the
component A is also rapidly rotating, as there is
apparently no correlation between directions of spin axes for wide
binaries (Howe & Clarke 2009).
6.1 Comparison with other visual binaries
HR 1847 is not the only example of a visual multiple system
with similar components, with some of them also showing the
Be phenomenon. The visual triple system Mon
consists of three Be stars
(see Marañón di Leo et al.
1994, and references therein), and all these three stars are
rapidly rotating (Abt et al. 2002).
The projected rotational velocities of
Mon A and
Mon C
was reported as 260
and 250
,
respectively, while
Mon B
is rotating more slowly (140
)
and, interestingly, also has weakest emission (Cowley
& Gugula 1973). This supports the connection between
rapid rotation and the Be phenomenon. More visual binaries
with Be-components may be found in Abt
& Cardona (1984).
Investigation of such multiple systems with resolved visual
components (like HR 1847 or Mon) may help when
studying multiple partially resolved or unresolved systems with Be
stars like o And
(see Olevic & Cvetkovic 2006,
and references therein) or
Cep (see Wheelwright et al. 2009,
and references therein), where light from all stars is mixed, making
the analysis extremely difficult.
The physical parameters and system characteristics derived from
resolved systems will put constraints on stellar structure and binary
evolution models, such that the unresolved systems can be modelled in a
better way with the improved models. Careful study of resolved systems
and careful determination of their parameters are very important
feedback on models.
7 Conclusions
This paper is the first attempt to collect all available information
about the stars in the visual binary system HR 1847
and to correct errors that appear in the SIMBAD database and Bright
Star Catalogue. We have presented results of our spectroscopic
analysis. HR 1847A (V=6.09, Shatskii 1998) is
a B type single-lined, eccentric, (e=0.70 0.02),
spectroscopic binary with a period of 719.79
0.17 days.
Model atmosphere analysis of this star yielded
,
,
and
.
HR 1847B (V=6.51, Shatskii
1998) is a Be star with variable radial
velocities, however, no reasonable orbital solution could be
found based on the available data. Model atmosphere analysis of this
star yielded the same effective temperature and surface gravity as for
the A component, but with a
rotational velocity of
.
A decrease in the
emission
was recorded during the last 4.5 years of observations.
In addition, positions of X-ray
(1RXS J053214.9+170319, see Sect. 2.8) and infrared
(X0501+589, see Sect. 2.9)
sources indicate that HR 1847B is more likely an X-ray and
IR source than HR 1847A.
Several other issues, such as the short term variability of HR 1847A or the reliable period determination of HR 1847B, could not be addressed by this paper owing to the lack of necessary data. Consequently, further long-term observations of these stars are desirable. Future work should also include a detailed abundance analysis using high S/N spectra and NLTE model atmospheres.
AcknowledgementsThe authors would like to devote this paper to the memory of Dr. Izold Pustylnik, with whom they consulted for the history of Struve's observations in Tartu. The authors would also like to thanks Zdenek Janák, Jan Elner, and Petr Svarícek for their help in early stages of the work. This research made use of the Washington Double Star Catalog maintained at the US Naval Observatory. This research has made use of the NASA's Astrophysics Data System Abstract Service. Our work was supported by a grant of the Grant Agency of the Czech Republic 205/08/0003. The Astronomical Institute Ondrejov is supported by project AV0 Z10030501.
References
- Abbott, D. C. 1980, ApJ, 242, 1183 [NASA ADS] [CrossRef] [Google Scholar]
- Abt, H. A., & Cardona, O. 1984, ApJ, 285, 190 [NASA ADS] [CrossRef] [Google Scholar]
- Abt, H. A., Levato, H., & Grosso, M. 2002, ApJ, 573, 359 [NASA ADS] [CrossRef] [Google Scholar]
- Andrews, P. J. 1968, MemRAS, 72, 35 [Google Scholar]
- Breger, M. 1990, A&A, 240, 308 [NASA ADS] [Google Scholar]
- Berghöfer, T. W., Schmitt, J. H. M. M., & Cassinelli, J. P. 1996, A&AS, 118, 481 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Berghöfer, T. W., Schmitt, J. H. M. M., Danner, R., & Cassinelli, J. P. 1997, A&A, 322, 167 [NASA ADS] [Google Scholar]
- Cannon, A. J. 1912a, Ann. Harvard College Observatory, 56, 65 [NASA ADS] [Google Scholar]
- Cannon, A. J. 1912b, Ann. Harvard College Observatory, 56, 227 [NASA ADS] [Google Scholar]
- Cannon, A. J., & Pickering, E. C. 1918, Ann. Harvard College Observatory, 92, 1 [Google Scholar]
- Coté, J., & Waters, L. B. F. M. 1987, A&A, 176, 93 [NASA ADS] [Google Scholar]
- Cowley, A., & Gugula, E. 1973, A&A, 22, 203 [NASA ADS] [Google Scholar]
- Cowley, A., Cowley, C., Jaschek, M., & Jaschek, C. 1969, AJ, 74, 375 [NASA ADS] [CrossRef] [Google Scholar]
- Donati, J.-F., Semel, M., Carter, B. D., Rees, D. E., & Collier Cameron, A. 1997, MNRAS, 291, 658 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
- Duflot, M., Fehrenbach, C., Mannone, C., Burnage, R., & Genty, V. 1992, A&AS, 110, 177 [Google Scholar]
- Eggen, O. J. 1977, PASP, 89, 205 [NASA ADS] [CrossRef] [Google Scholar]
- Fabricius, C., Høg, E., Makarov, V. V., et al. 2002, A&A, 384, 180 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Flesch, E., & Hardcastle, M. J. 2004, A&A, 427, 387 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Frost, E. B., Barrett, S. B., & Struve, O. 1926, ApJ, 64, 1 [NASA ADS] [CrossRef] [Google Scholar]
- Gahm, G. F., Ahlin, P., & Lindroos, K. P. 1983, A&AS, 51, 143 [Google Scholar]
- Gray, D. F. 1976, The observation and analysis of stellar photospheres (New York: John Wiley & Sons) [Google Scholar]
- Hadrava, P. 1990, Contrib. Astron. Obs. Skalnaté Pleso, 20, 23 [Google Scholar]
- Hadrava, P. 2004, Publ. Astron. Inst. ASCR, 92, 1 [Google Scholar]
- Herschel, W. 1785, Phil. Trans. Roy. Soc. London, 75, 40 [CrossRef] [Google Scholar]
- Herschel, W. 1821, Mem. Astron. Soc., 1, 166 [Google Scholar]
- Hoffleit, D., & Jaschek, C. 1991, The Bright Star Catalogue, 5th Revised Ed. (New Haven: Yale University Observatory) [Google Scholar]
- Horn, J., Kubát, J., Harmanec, P., et al. 1996, A&A, 309, 521 [NASA ADS] [Google Scholar]
- Howe, K. S., & Clarke, C. J. 2009, MNRAS, 392, 448 [NASA ADS] [CrossRef] [Google Scholar]
- Hubert, A.-M. 2007, in Active OB-Stars: Laboratories for Stellar & Circumstellar Physics, ed. S. Stefl, S. P. Owocki, & A. T. Okazaki, ASP Conf. Ser., 361, 27 [Google Scholar]
-
Iwata, I., Okumura, S., & Sait
, M. 1999, PASJ, 51, 653 [NASA ADS] [Google Scholar]
- Kaufer, A. 1998, Rev. Mod. Astron., 11, 177 [NASA ADS] [Google Scholar]
- Kharchenko, N. V. 2001, Kin. Fiz. Neb. Tel, 17, 409 [Google Scholar]
- Kharchenko, N. V., Piskunov, A. E., Roeser, S., Schilbach, E., & Scholz, R.-D. 2004, AN, 325, 740 [NASA ADS] [Google Scholar]
- Kubát, J., Saad, S. M., Slechta, M., & Yang, S. 2010, in Binaries - Key to Comprehension of the Universe, ed. A. Prsa, & M. Zejda, ASP Conf. Ser., in press [Google Scholar]
- Kurucz, R. L. 1993, ATLAS9 Stellar Atmosphere Programs and 2 km s-1 grid, Kurucz CD-ROM No. 13 [Google Scholar]
- Levato, H. 1975, A&A, 19, 91 [Google Scholar]
- Lindroos, K. P. 1983, A&AS, 51, 161 [Google Scholar]
- Magnier, E. A., Volp, A. W., Laan, K., van den Ancker, M. E., & Waters, L. B. F. M. 1999, A&A, 352, 228 [NASA ADS] [Google Scholar]
- Marañón di Leo, C., Colombo, E., & Ringuelet, A. E. 1994, A&A, 286, 160 [NASA ADS] [Google Scholar]
- Mason, B. D., Hartkopf, W. I., Wycoff, G. L., et al. 2004, AJ, 127, 539 [NASA ADS] [CrossRef] [Google Scholar]
- Mora, A., Merín, B., Solano, E., et al. 2001, A&A, 378, 116 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Olevic, D., & Cvetkovic, Z. 2006, AJ, 131, 1721 [NASA ADS] [CrossRef] [Google Scholar]
- Osawa, K. 1959, ApJ, 130, 159 [NASA ADS] [CrossRef] [Google Scholar]
- Oudmaijer, R. D., Palacios, J., Eiroa, C., et al. 2001, A&A, 379, 564 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Percy, J. R., Harlow, C. D. W., & Wu, A. P. S. 2004, PASP, 116, 178 [NASA ADS] [CrossRef] [Google Scholar]
- Perryman, M. A. C., & ESA 1997, The Hipparcos and Tycho catalogues, ESA, Noordwijk, ESA SP Ser., 1200 [Google Scholar]
- Plaskett, J. S. 1919, JRASC, 13, 197 [NASA ADS] [Google Scholar]
- Plaskett, J. S., & Young, R. K. 1919, JRASC, 13, 191 [Google Scholar]
- Plaskett, J. S., Harper, W. E., Young, R. K., & Plaskett, H. H. 1920, Publ. Dominion Astrophys. Obs., 1, 163 [NASA ADS] [Google Scholar]
- Porter, J. M., & Rivinius, Th. 2003, PASP, 115, 1153 [NASA ADS] [CrossRef] [Google Scholar]
- Russell, H. N., & Moore, C. E. 1929, AJ, 39, 165 [NASA ADS] [CrossRef] [Google Scholar]
- Shatskii, N. I. 1998, PAZh, 24, 307, Astron. Lett., 24, 257 [Google Scholar]
- Skoda, P. 1996, in Astronomical Data Analysis Software and Systems V, ed. G. H. Jacoby, & J. Barnes, ASP Conf. Ser., 101, 187 [Google Scholar]
- Skoda, P., & Slechta, M. 2002, Publ. Astron. Inst. ASCR, 90, 40 [Google Scholar]
- Skrutskie, M. F., Cutri, R. M., Stiening, R., et al. 2006, AJ, 131, 1163 [NASA ADS] [CrossRef] [Google Scholar]
- Slettebak, A. 1963, ApJ, 138, 118 [NASA ADS] [CrossRef] [Google Scholar]
- Stahl, O., Kaufer, A., Wolf, B., et al. 1995, J. Astron. Data, 1, 3 [Google Scholar]
- Stellingwerf, R. F. 1978, ApJ, 224, 953 [NASA ADS] [CrossRef] [Google Scholar]
- Struve, F. G. W. 1837, Stellarum Duplicium et Multiplicium Mensurae Micrometricae, Ex Typographia Academica, Petropoli [Google Scholar]
- Theodossiou, E., & Danezis, E. 1991, Ap&SS, 183, 91 [NASA ADS] [CrossRef] [Google Scholar]
- van Leeuwen, F. 2007, A&A, 474, 653 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Vieiria, S. L. A., Corradi, W. J. B., Alencar, S. H. P., et al. 2003, AJ, 126, 2971 [NASA ADS] [CrossRef] [Google Scholar]
- Voges, W., Aschenbach, B., & Boller, Th. 2000, IAUC, 7432, 15944 [Google Scholar]
- Wackerling, L. R. 1970, PASP, 82, 1357 [NASA ADS] [CrossRef] [Google Scholar]
- Wheelwright, H. E., Oudmaijer, R. D., & Schnerr, R. S. 2009, MNRAS, 497, 487 [Google Scholar]
- Whitelock, P. A., Feast, M. W., & Catchpole, R. M. 1989, MNRAS, 238, 7 [NASA ADS] [Google Scholar]
- Zhang, E.-H., Robinson, E. L., & Nather, R. E. 1986, ApJ, 305, 740 [NASA ADS] [CrossRef] [Google Scholar]
Online Material
Appendix A: Visual spectra of HR 1847A and HR 1847B
![]() |
Figure A.1:
Line identification of the spectrum of HR 1847A obtained with
the blue channel of the HEROS spectrograph (dots)
and comparison with the synthetic spectrum calculated from the Kurucz (1993)
LTE model atmosphere |
Open with DEXTER |
![]() |
Figure A.1: continued. |
Open with DEXTER |
![]() |
Figure A.2:
Line identification of the spectrum of HR 1847A obtained with
the red channel of the HEROS spectrograph (dots)
and comparison with the synthetic spectrum calculated from the Kurucz (1993)
LTE model atmosphere |
Open with DEXTER |
![]() |
Figure A.3:
Line identification of the spectrum of HR 1847B obtained with
the blue channel of the HEROS spectrograph (dots)
and comparison with a synthetic spectrum calculated from the Kurucz (1993)
LTE model atmosphere |
Open with DEXTER |
![]() |
Figure A.3: continued. |
Open with DEXTER |
![]() |
Figure A.4:
Line identification of the spectrum of HR 1847B obtained with
the red channel of the HEROS spectrograph (dots),
and comparison with a synthetic spectrum calculated from the Kurucz (1993)
LTE model atmosphere |
Open with DEXTER |
Table A.1:
Heliocentric radial velocities (RV) of HR 1847A - spectra from
Ondrejov Observatory, where
is the heliocentric velocity.
Table A.2: Heliocentric radial velocities (RV) of HR 1847A - spectra from Rozhen Observatory.
Table A.3: Heliocentric radial velocities (RV) of HR 1847B - spectra from Ondrejov Observatory.
Table A.4: Heliocentric radial velocities (RV) of HR 1847B - spectra from Rozhen Observatory.
Footnotes
- ... HR 1847
- Based on observations with the Ondrejov and Rozhen 2-m telescopes.
- ...
- Appendix is only available in electronic form at http://www.aanda.org
- ... WEBDA
- The Galactic and Magellanic Clouds open cluster database WEBDA is available at http://obswww.unige.ch/webda/
- ... IRAF
- IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation.
All Tables
Table 1:
HIPPARCOS and
photometry of HR 1847.
Table 2: Candidate frequencies resulting from the PDM period search.
Table 3: Orbital elements of HR 1847A with FOTEL.
Table 4: Summary of parameters of both components of HR 1847.
Table A.1:
Heliocentric radial velocities (RV) of HR 1847A - spectra from
Ondrejov Observatory, where
is the heliocentric velocity.
Table A.2: Heliocentric radial velocities (RV) of HR 1847A - spectra from Rozhen Observatory.
Table A.3: Heliocentric radial velocities (RV) of HR 1847B - spectra from Ondrejov Observatory.
Table A.4: Heliocentric radial velocities (RV) of HR 1847B - spectra from Rozhen Observatory.
All Figures
![]() |
Figure 1:
The radial velocity variations for hydrogen |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
Upper panel: power spectrum of measured RVs
of |
Open with DEXTER | |
In the text |
![]() |
Figure 3:
Phase diagram of measured RVs for |
Open with DEXTER | |
In the text |
![]() |
Figure 4:
Upper panel: radial velocity curve of the
primary component corresponding to the FOTEL
orbital solution III (
|
Open with DEXTER | |
In the text |
![]() |
Figure 5:
The evolution of the |
Open with DEXTER | |
In the text |
![]() |
Figure 6:
Time evolution of the |
Open with DEXTER | |
In the text |
![]() |
Figure A.1:
Line identification of the spectrum of HR 1847A obtained with
the blue channel of the HEROS spectrograph (dots)
and comparison with the synthetic spectrum calculated from the Kurucz (1993)
LTE model atmosphere |
Open with DEXTER | |
In the text |
![]() |
Figure A.1: continued. |
Open with DEXTER | |
In the text |
![]() |
Figure A.2:
Line identification of the spectrum of HR 1847A obtained with
the red channel of the HEROS spectrograph (dots)
and comparison with the synthetic spectrum calculated from the Kurucz (1993)
LTE model atmosphere |
Open with DEXTER | |
In the text |
![]() |
Figure A.3:
Line identification of the spectrum of HR 1847B obtained with
the blue channel of the HEROS spectrograph (dots)
and comparison with a synthetic spectrum calculated from the Kurucz (1993)
LTE model atmosphere |
Open with DEXTER | |
In the text |
![]() |
Figure A.3: continued. |
Open with DEXTER | |
In the text |
![]() |
Figure A.4:
Line identification of the spectrum of HR 1847B obtained with
the red channel of the HEROS spectrograph (dots),
and comparison with a synthetic spectrum calculated from the Kurucz (1993)
LTE model atmosphere |
Open with DEXTER | |
In the text |
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