279 research outputs found
Notes on the disentangling of spectra I. Enhancement in precision
Context: The technique of disentangling has been applied to numerous
high-precision studies of spectroscopic binaries and multiple stars. Although,
its possibilities have not yet been fully understood and exploited. Aims:
Theoretical background aspects of the method, its latest improvements and hints
for its use in practice are explained in this series of papers. Methods: In
this first paper of the series, we discuss spectral-resolution limitations due
to a discrete representation of the observed spectra and introduce a new method
how to achieve a precision higher than the step of input-data binning. Results:
Based on this principle, the latest version of the KOREL code for Fourier
disentangling achieves an increase in precision for an order of magnitude.Comment: 2 figure
The radial velocity curve of HD153919 (4U1700-37) revisited
We have re-analysed all available high-resolution ultraviolet IUE spectra of
the high-mass X-ray binary HD153919/4U1700-37. The radial velocity
semi-amplitude of 20.6 +/- 1.0 km/s and orbital eccentricity of 0.22 +/- 0.04
agree very well with the values obtained earlier from optical spectra. They
disagree with earlier conclusions for the same data reduced by Heap & Corcoran
(1992) and by Stickland & Lloyd (1993).Comment: 6 pages, latex, figure included, Astronomy & Astrophysics, in pres
New distance and depth estimates from observations of eclipsing binaries in the SMC
A sample of 33 eclipsing binaries observed in a field of the SMC with
FLAMES@VLT is presented. The radial velocity curves obtained, together with
existing OGLE light curves, allowed the determination of all stellar and
orbital parameters of these binary systems. The mean distance modulus of the
observed part of the SMC is 19.05, based on the 26 most reliable systems.
Assuming an average error of 0.1 mag on the distance modulus to an individual
system, and a gaussian distribution of the distance moduli, we obtain a 2-sigma
depth of 0.36 mag or 10.6 kpc. Some results on the kinematics of the binary
stars and of the H II gas are also given.Comment: 6 pages, 4 figures, Proc. IAU Symp. No 256, The Magellanic System:
Stars, Gas and Galaxies, eds. Jacco Th. van Loon & Joana M. Oliveir
Quantitative spectroscopy of close binary stars
The method of spectral disentangling has now created the opportunity for
studying the chemical composition in previously inaccessible components of
binary and multiple stars. This in turn makes it possible to trace their
chemical evolution, a vital aspect in understanding the evolution of stellar
systems. We review different ways to reconstruct individual spectra from
eclipsing and non-eclipsing systems, and then concentrate on some recent
applications to detached binaries with high-mass and intermediate-mass stars,
and Algol-type mass-transfer systems.Comment: To appear in the Proceedings of IAU Symposium 282 'From Interacting
Binaries to Exoplanets: Essential Modeling Tools
Absolute Dimensions and Apsidal Motion of the Young Detached System LT Canis Majoris
New high resolution spectra of the short period (P~1.76 days) young detached
binary LT CMa are reported for the first time. By combining the results from
the analysis of new radial velocity curves and published light curves, we
determine values for the masses, radii and temperatures as follows: M_1= 5.59
(0.20) M_o, R_1=3.56 (0.07) R_o and T_eff1= 17000 (500) K for the primary and
M_2=3.36 (0.14) M_o, R_2= 2.04 (0.05) R_o and T_eff2= 13140 (800) K for the
secondary. Static absorbtion features apart from those coming from the close
binary components are detected in the several spectral regions. If these
absorbtion features are from a third star, as the light curve solutions
support, its radial velocity is measured to be RV_3=70(8) km s^-1. The orbit of
the binary system is proved to be eccentric (e=0.059) and thus the apsidal
motion exists. The estimated linear advance in longitude of periastron
corresponds to an apsidal motion of U=694+/-5 yr for the system. The average
internal structure constant log k_2,obs=-2.53 of LT CMa is found smaller than
its theoretical value of log k_2,theo=-2.22 suggesting the stars would have
more central concentration in mass. The photometric distance of LT CMa
(d=535+/-45 pc) is found to be much smaller than the distance of CMa OB1
association (1150 pc) which rules out membership. A comparison with current
stellar evolution models for solar metallicity indicates that LT CMa (35 Myr)
is much older than the CMa OB1 association (3 Myr), confirming that LT CMa is
not a member of CMa OB1. The kinematical and dynamical analysis indicate LT CMa
is orbiting the Galaxy in a circular orbit and belongs to the young thin-disk
population.Comment: 19 pages, 6 figures and 6 tables, accepted for publication in
Publication of the Astronomical Society of Japa
Abundances from disentangled component spectra: the eclipsing binary V578 Mon
Chemical abundances of the early-B type components of the binary V578 Mon are
derived from disentangled component spectra. This is a pilot study showing
that, even with moderately high line-broadening, metal abundances can be
derived from disentangled spectra with a precision 0.1 dex, relative to
sharp-lined single stars of the same spectral type. This binary is well-suited
for such an assessment because of its youth as a member of the Rosette Nebula
cluster NGC 2244, strengthening the expectation of an unevolved ZAMS chemical
composition. The method is of interest to study rotational driven mixing in
main-sequence stars, with fundamental stellar parameters known with higher
accuracy in (eclipsing) binaries. The paper also includes an evaluation of the
bias that might be present in disentangled spectra.Comment: Accepted for publication in Astronomy & Astrophysics, 8 pages, 2
figure
Spectra disentangling applied to the Hyades binary Theta^2 Tau AB: new orbit, orbital parallax and component properties
Theta^2 Tauri is a detached and single-lined interferometric-spectroscopic
binary as well as the most massive binary system of the Hyades cluster. The
system revolves in an eccentric orbit with a periodicity of 140.7 days. The
secondary has a similar temperature but is less evolved and fainter than the
primary. It is also rotating more rapidly. Since the composite spectra are
heavily blended, the direct extraction of radial velocities over the orbit of
component B was hitherto unsuccessful. Using high-resolution spectroscopic data
recently obtained with the Elodie (OHP, France) and Hermes (ORM, La Palma,
Spain) spectrographs, and applying a spectra disentangling algorithm to three
independent data sets including spectra from the Oak Ridge Observatory (USA),
we derived an improved spectroscopic orbit and refined the solution by
performing a combined astrometric-spectroscopic analysis based on the new
spectroscopy and the long-baseline data from the Mark III optical
interferometer. As a result, the velocity amplitude of the fainter component is
obtained in a direct and objective way. Major progress based on this new
determination includes an improved computation of the orbital parallax. Our
mass ratio is in good agreement with the older estimates of Peterson et al.
(1991, 1993), but the mass of the primary is 15-25% higher than the more recent
estimates by Torres et al. (1997) and Armstrong et al. (2006). Due to the
strategic position of the components in the turnoff region of the cluster,
these new determinations imply stricter constraints for the age and the
metallicity of the Hyades cluster. The location of component B can be explained
by current evolutionary models, but the location of the more evolved component
A is not trivially explained and requires a detailed abundance analysis of its
disentangled spectrum.Comment: in press, 13 pages, 10 Postscript figures, 5 tables. Table~4 is
available as online material. Keywords: astrometry - techniques: high angular
resolution - stars: binaries: visual - stars: binaries: spectroscopic -
stars: fundamental parameter
Tehnike razdvajanja za raspetljavanje složenih spektara
Disentangling of composite spectra is a promissing technique for the analysis of double-lined spectroscopic binary systems. The technique makes use of a separation routine to extract model-component spectra out of a time series of observed composite spectra. Focusing on the differences between two possible approaches in the implementation of the separation routine, we compare the resulting limitations. We perform test runs on artificial data and conclude that separation in the wavelength domain is more versatile in several aspects, while the computational efficiency of separation in the Fourier domain allows working with larger data sets which is beneficial in a fully-blown disentangling process.Raspetljavanje složenih spektara je obećavajuća metoda za proučavanje dvojnih zvjezdanih sustava. Ta metoda primjenjuje rutinu za razdvajanje kojom se izlučuje spektre zvijezda komponenata modela iz vremenskog niza opaženih složenih spektara. Usredotočujući se na razlike u pristupu pri izvedbi rutine za rastavljanje, uspoređujemo ograničenja koja iz njih proizlaze. Proveli smo ispitivanje s umjetnim podacima i zaključili da je rastavljanje u području valnih duljina svestranije u više pogleda, dok rastavljanje primjenom Fourierovog transformata dozvoljava rad s većim skupovima podataka, što je povoljno u potpunom procesu raspetljavanja složenih spektara
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