Orbital motions and light curves of young binaries XZ Tau and VY Tau

Autor: A. V. Zharova, S. A. Lamzin, E. V. Malogolovets, N. V. Emelyanov, J. M. Roe, A. V. Dodin
Přispěvatelé: Sternberg Astronomical Institute [Moscow], Lomonosov Moscow State University (MSU), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Jazyk: angličtina
Rok vydání: 2016
Předmět:
Zdroj: Astronomy Letters / Pis'ma v Astronomicheskii Zhurnal
Astronomy Letters / Pis'ma v Astronomicheskii Zhurnal, 2016, 42 (1), pp.29-40. ⟨10.1134/S1063773716010035⟩
Astronomy Letters / Pis'ma v Astronomicheskii Zhurnal, MAIK Nauka/Interperiodica, 2016, 42 (1), pp.29-40. ⟨10.1134/S1063773716010035⟩
ISSN: 1063-7737
1562-6873
DOI: 10.1134/S1063773716010035⟩
Popis: The results of our speckle interferometric observations of young binaries VY Tau and XZ Tau are presented. For the first time, we found a relative displacement of VY Tau components as well as a preliminary orbit for XZ Tau. It appeared that the orbit is appreciably non-circular and is inclined by $i \lesssim 47^o$ from the plane of the sky. It means that the rotation axis of XZ Tau A and the axis of its jet are significantly non-perpendicular to the orbital plane. We found that the average brightness of XZ Tau had been increasing from the beginning of the last century up to the mid-thirties and then it decreased by $\Delta B > 2$ mag. The maximal brightness has been reached significantly later on the time of periastron passage. The total brightness of XZ Tau's components varied in a non-regular way from 1970 to 1985 when eruptions of hot gas from XZ Tau A presumably had occurred. In the early nineties the variations became regular following which a chaotic variability had renewed. We also report that a flare activity of VY Tau has resumed after 40 yr pause, parameters of the previous and new flares are similar, and the flares are related with the A component.
Comment: 18 pages, 4 figures, accepted for publication in the Astronomy Letters
Databáze: OpenAIRE
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