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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{AA8637f1.eps}\end{figure}$ Figure 1: Orbit of the young stellar binary system V773 Tau based on the interferometric-spectroscopic model by Boden & collaborators (2007). The secondary is given at our seven (A-G) VLBI observations (epoch 2004) and at Phillips & collaborators (1996) VLBI observation (epoch 1992). Stellar diameters are rendered to scale.
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In the text

$\begin{figure} \par\includegraphics[width=15.45cm,clip]{aa8637_fig2.eps.CMJN.eps}\end{figure}$ Figure 2: Seven consecutive 8.4 GHz VLBA+EB images of the young stellar binary system V773 Tau A. Stellar positions are indicated by crosses. Starting with panel A, the peak flux density in the images are 0.1, 0.5, 0.5, 0.2, 0.7, 0.2, 0.5 mJy/beam. Contour levels are -1, 1, 1.5, 2, 2.5, 3, 4 and 5 times the 3 $\sigma$ (0.1 mJy/beam). The beam size is shown in the bottom right corner of each panel (average beam size: 1.3 $\times$ 0.5 mas). The sketch of the system, not to scale, shows helmet streamers, i.e. structures formed by a helmet located on top of a coronal loop anchored on a rotating star, and a very large streamer. The topology is here simplified, for each star are only drawn two streamers of a possible solar-like streamer belt.
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In the text

$\begin{figure} \par\includegraphics[width=13.8cm,clip]{AA8637f3.eps}\end{figure}$ Figure 3: Flux density versus time. Top panel: flux density of the SW radio structures (associated with the primary star) in the VLBA+EB maps. Filled circles express the combined flux of helmets and upper mirror points; empty circles indicate that only helmets are present. Middle panel: flux density of the NE radio structures (associated with the secondary star). Filled squares when helmets and upper mirrors are both present, empty squares when only helmets are present. Bottom panel: total flux density measured with the Effelsberg 100-m telescope outside the VLBA+EB observing time. The points which are likely to belong to the same flaring event have been connected (days 5-6).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{AA8637f1.eps}\end{figure}$	Figure 1: Orbit of the young stellar binary system V773 Tau based on the interferometric-spectroscopic model by Boden & collaborators (2007). The secondary is given at our seven (A-G) VLBI observations (epoch 2004) and at Phillips & collaborators (1996) VLBI observation (epoch 1992). Stellar diameters are rendered to scale.
Open with DEXTER