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An active binary XY UMa revisited

By T. Pribulla, D. Chochol, P. A. Heckert, L. Errico, A. A. Vittone, Š. Parimucha and M. Teodorani

Abstract

New extensive multicolour photoelectric photometry, performed since 1994, is presented. 17 more-or-less complete light curves were obtained and analyzed. The Wilson-Devinney code applied to the BVRI light curves without the maculation effect together with published spectroscopic mass ratio and semi-major axis yielded new absolute parameters of the eclipsing pair: $m_1 = 1.10 M_{\odot}$, $m_2 = 0.66 M_{\odot}$, $R_1 = 1.16 R_{\odot}$, $R_2 = 0.63 R_{\odot}$, $a = 3.107 R_{\odot}$ and the orbital inclination $i = 80.9\degr$. The observed orbital period changes are conclusively explained by the mutual action of the third body in the system ($P_3 = 30$ years) and the maculation effects. Simultaneous analysis of the period changes and the visual brightness excludes the possibility of their explanation by Applegate's mechanism. The differences in the maxima heights caused by the maculation exhibit variations with the period of $709 \pm 10$ days. The distance to the system $d = 86 \pm 5$ pc determined from the absolute dimensions and luminosities of the components is larger than the Hipparcos astrometric value $d = 66 \pm 6$ pc

Topics: stars: binaries eclipsing, stars: individual: XY UMa, stars: pre-main sequence, stars: magnetic fields
Publisher: EDP Sciences
DOI identifier: 10.1051/0004-6361:20010459/pdf
OAI identifier: oai:edpsciences.org:dkey/10.1051/0004-6361:20010459
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