| JANÍK, J., P. HARMANEC, H. LEHMANN, S. YANG, H. BOŽIČ, H. AK, P. HADRAVA, P. EENENS, D. RUŽDJAK, D. SUDAR, I. HUBENÝ and A.P. LINNELL. Search for forced oscillations in binaries. IV. The eclipsing binary V436 Per revisited. Astronomy and Astrophysics. Les Ulis Cedex, France: EDP Sciences, 2003, vol. 2003, No 408, p. 611-619. ISSN 0004-6361. |
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@article{489291,
author = {Janík, J. and Harmanec, P. and Lehmann, H. and Yang, S. and Božič, H. and Ak, H. and Hadrava, P. and Eenens, P. and Ruždjak, D. and Sudar, D. and Hubený, I. and Linnell, A.P.},
article_location = {Les Ulis Cedex, France},
article_number = {408},
keywords = {binaries stars; eclipsing stars; spectroscopic stars; fundamental parameters; oscillations;},
language = {eng},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
title = {Search for forced oscillations in binaries. IV. The eclipsing binary V436 Per revisited},
volume = {2003},
year = {2003}
}
TY - JOUR
ID - 489291
AU - Janík, J. - Harmanec, P. - Lehmann, H. - Yang, S. - Božič, H. - Ak, H. - Hadrava, P. - Eenens, P. - Ruždjak, D. - Sudar, D. - Hubený, I. - Linnell, A.P.
PY - 2003
TI - Search for forced oscillations in binaries. IV. The eclipsing binary V436 Per revisited
JF - Astronomy and Astrophysics
VL - 2003
IS - 408
SP - 611-619
EP - 611-619
PB - EDP Sciences
SN - 00046361
KW - binaries stars
KW - eclipsing stars
KW - spectroscopic stars
KW - fundamental parameters
KW - oscillations;
N2 - An analysis of new spectroscopic and photoelectric U B V observations, satisfactorily covering the whole orbital period of V436 Per, together with existing data allowed us to improve the knowledge of the basic physical characteristics of the binary and its components. In several aspects, our new results differ from the findings of Paper I of this series: in particular, we found that it is the star eclipsed in the secondary minimum which is slightly more massive and larger than the optical primary. We also conclude that the apsidal advance - if present at all - is much slower than that estimated in a previous study. The orbital period might be increasing by 0.28 s per year but also this finding is very uncertain and needs verification by future observations. It is encouraging to note that two completely independent sets of programs for light-curve solutions lead to identical results. A notable finding is that both binary components rotate with very similar - if not identical - rotational periods of 1d.45 and 1d.40, much shorter than what would correspond to a 10d.9 spin-orbit synchronization period at periastron. Rapid line-profile changes reported earlier could not be confirmed from new, dedicated series of high-resolution and S/N spectra.
ER -
JANÍK, J., P. HARMANEC, H. LEHMANN, S. YANG, H. BOŽIČ, H. AK, P. HADRAVA, P. EENENS, D. RUŽDJAK, D. SUDAR, I. HUBENÝ and A.P. LINNELL. Search for forced oscillations in binaries. IV. The eclipsing binary V436 Per revisited. \textit{Astronomy and Astrophysics}. Les Ulis Cedex, France: EDP Sciences, 2003, vol.~2003, No~408, p.~611-619. ISSN~0004-6361.
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