Issue |
A&A
Volume 422, Number 3, August II 2004
|
|
---|---|---|
Page(s) | 1013 - 1021 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20040253 | |
Published online | 16 July 2004 |
Disentangling component spectra of , a spectroscopic binary with a pulsating primary *
I. Improved physical elements and analysis of periodic rapid variations of scalar quantities
1
Astronomical Institute of the Charles University, V Holešovičkách 2, 18000 Praha 8, Czech Republic e-mail: hec@sunstel.asu.cas.cz
2
Astronomical Institute, Academy of Sciences, 25165 Ondřejov, Czech Republic
3
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, 3001 Leuven, Belgium
Received:
12
February
2004
Accepted:
11
April
2004
A new reduction and a new analysis of a rich series of high-S/N
spectra of the bright star is carried out to test
the technique of spectral disentangling in the case when one of the components
is a non-radial oscillator. We improve the orbital elements of the system and
find the basic physical properties of the binary to be Teff = 24 500 K,
masses of 10.7–11.9 and 9.6–10.7
and the primary
radius and rotational period of 7–8
and 3
56–3
68, respectively.
This also implies log g = 3.70–3.78 [cgs].
KOREL disentangling is applied and we find
that it worked properly and was not misled by the complex line-profile
variability of the pulsating primary. Moreover, the pulsational frequencies
are detected via the period search in the line intensities and radial-velocity
residuals of the primary derived by KOREL
and in the time series of residual spectra in the rest frame of the primary
after KOREL disentangling. This constitutes a much better starting point
to interpret the complex pixel-by-pixel variations of the disentangled
profiles of the primary in terms of stellar oscillations and/or additional
rotational modulation than the original spectra before disentangling.
Key words: stars: binaries: spectroscopic / stars: oscillations / line: profiles / stars: individual:
© ESO, 2004
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