Abstract
The quadruple young system GG Tauri is an example of a multiple T Tauri system. Its consists of two binaries, the brighter one ( GG Tau A) being surrounded by a ring-shape circumbinary disk. In a recent paper, we performed a dynamical study of circumbinary and showed that there is an apparent discrepancy between the orbital fit of GG Tau A and the observed inner edge of the disk. In this paper, we now investigate the dynamics of the whole quadruple system together with the disk. We show that it is possible to design an orbital configuration between the two binaries in such a way that the outer profile of the circumbinary ring may be explained by tidal interaction with repeated periastron passages of the outer binary GG Tau B. We show that the observed characteristics of the disk are not compatible with some orbital configurations, such as those giving rise to the Kozai resonance. Surprisingly, the outer binary GG Tau B appears only marginally stable against tidal disruption by GG Tau A. GG Tau B appears stable only if its internal orbit is retrograde with respect to the motion of its center of mass around GG Tau A. We also find that the CB disk should be almost coplanar with the inner binary.
Highlights
GG Tauri is a quadruple T Tauri systems consisting of two binaries
We performed a dynamical study of circumbinary and showed that there is an apparent discrepancy between the orbital fit of GG Tau A and the observed inner edge of the disk
We show that it is possible to design an orbital configuration between the two binaries in such a way that the outer profile of the circumbinary ring may be explained by tidal interaction with repeated periastron passages of the outer binary GG Tau B
Summary
GG Tauri is a quadruple T Tauri systems consisting of two binaries. The first pair (GG Tau A) is brighter and closer (0.25 ). The second pair (GG Tau B) is wider (1.48 ) and located 10.1 to the south (Guilloteau et al 1999, hereafter GDS99; White et al 1999). GG Tau A is well known to be surrounded by a circumbinary dusty and gaseous disk that was spatially resolved in both millimeter and near infrared wavelength domains (Dutrey et al 1994; GDS99). This disk is the prototype example of a circumbinary disk in a young stellar system. The total mass of the circumbinary material (H2 + dust) is ∼0.12 M (GDS99)
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