Browsing by Author "Zurlo, A."

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    Characterization of low-mass companion HD 142527 B
    (2018) Christiaens, V.; Casassus, S.; Absil, O.; Kimeswenger, S.; Gonzalez, C. A. Gomez; Girard, J.; Ramirez, R.; Wertz, O.; Zurlo, A.; Wahhaj, Z.; Flores, C.; Salinas, V.; Jordán Colzani, Andrés Cristóbal; Mawet, D.
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    Ongoing flyby in the young multiple system UX Tauri
    (2020) Menard, F.; Cuello, N.; Ginski, C.; van der Plas, G.; Villenave, M.; Gonzalez, J-F; Pinte, C.; Benisty, M.; Boccaletti, A.; Price, D. J.; Boehler, Y.; Chripko, S.; de Boer, J.; Dominik, C.; Garufi, A.; Gratton, R.; Hagelberg, J.; Henning, Th; Langlois, M.; Maire, A. L.; Pinilla, P.; Ruane, G. J.; Schmid, H. M.; van Holstein, R. G.; Vigan, A.; Zurlo, A.; Hubin, N.; Pavlov, A.; Rochat, S.; Sauvage, J-F; Stadler, E.
    We present observations of the young multiple system UX Tauri to look for circumstellar disks and for signs of dynamical interactions. We obtained SPHERE/IRDIS deep differential polarization images in the J and H bands. We also used ALMA archival CO data. Large extended spirals are well detected in scattered light coming out of the disk of UX Tau A. The southern spiral forms a bridge between UX Tau A and C. These spirals, including the bridge connecting the two stars, all have a CO (3-2) counterpart seen by ALMA. The disk of UX Tau C is detected in scattered light. It is much smaller than the disk of UX Tau A and has a major axis along a different position angle, suggesting a misalignment. We performed PHANTOM SPH hydrodynamical models to interpret the data. The scattered light spirals, CO emission spirals and velocity patterns of the rotating disks, and the compactness of the disk of UX Tau C all point to a scenario in which UX Tau A has been perturbed very recently (similar to 1000 years) by the close passage of UX Tau C.
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    The White Dwarf Binary Pathways Survey -III. Contamination from hierarchical triples containing a white dwarf
    (2020) Lagos, F.; Schreiber, M. R.; Parsons, S. G.; Zurlo, A.; Mesa, D.; Gansicke, B. T.; Brahm, R.; Caceres, C.; Canovas, H.; Hernandez, M-S; Jordan, A.; Koester, D.; Schmidtobreick, L.; Tappert, C.; Zorotovic, M.
    The White Dwarf Binary Pathways Survey aims at increasing the number of known detached A, F, G, and K main-sequence stars in close orbits with white dwarf companions (WD+AFGK binaries) to refine our understanding about compact binary evolution and the nature of Supernova Ia progenitors. These close WD+AFGK binary stars are expected to form through common envelope evolution, in which tidal forces tend to circularize the orbit. However, some of the identified WD+AFGK binary candidates show eccentric orbits, indicating that these systems are either formed through a different mechanism or perhaps they are not close WD+AFGK binaries. We observed one of these eccentric WD+AFGK binaries with SPHERE and find that the system TYC 7218-934-1 is in fact a triple system where the WD is a distant companion. The inner binary likely consists of the G-type star plus an unseen low-mass companion in an eccentric orbit. Based on this finding, we estimate the fraction of triple systems that could contaminate the WD+AFGK sample. We find that less than 15 per cent of our targets with orbital periods shorter than 100 d might be hierarchical triples.