All Figures

$\begin{figure} \par\includegraphics[angle=270,width=8.4cm,clip]{0866fig1.ps} \end{figure}$ Figure 1: The R Aqr jet in 8 GHz observed in 1999.78. The peak flux is 10.4 mJy. Contour levels are -0.06, 0.06, 0.12, 0.24, 0.48, 0.96, 1.92, 3.84, 7.68 mJy. The beam size is $780\times 540$ mas (PA $73\hbox {$^\circ $ }$ ) and the rms noise is 17 $\mu$ Jy. Lower contours are used here to show the outer low flux density areas. The crosses show the position of each component in 1992.83, except B and D in 1991.63 (LJ).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.4cm]{0866fig2.ps} \end{figure}$ Figure 2: The R Aqr jet in 8 GHz observed in 1992.83. The peak flux is 6.4 mJy. Contour levels are -0.17, 0.17, 0.33, 0.66, 1.32, 2.64 and 5.28 mJy. The beam size in this uniformly weighted map is $359\times 228$ mas (PA $31\hbox {$^\circ $ }$ ). Note the two parts in A (NE) and A $\hbox {$^\prime $ }$ (SW), the shock front in C2 and the SW extension in the core. The crosses show the positions of B and D in 1991.63 and in 1999.78.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=16.8cm,clip]{0866fig3.ps} \end{figure}$ Figure 3: The R Aqr jet in 22 GHz in 1992.83 a) and in 1999.78 b) showing the core region. Note that both maps are untapered. No new component can be seen emerging from the core unless it had already emerged before 1992 (see discussion in text). a) The peak flux is $7.37\times 10^{-3}$ Jy. Contours drawn are -0.25, 0.25, 0.60, 0.96, 1.31, 1.66, 2.02, 2.37, 2.73, 3.08, 3.43, 3.79, 4.14, 4.49, 4.85 and 5.20 mJy. The beam size in this uniform weighted map is $159 \times 121$ mas (PA $1{\hbox{$.\!\!^\circ$ }}3$ ) and the rms noise is 100 $\mu$ Jy. The integral intensities of C1c, C1b and C1a are 10.11, 7.32 and 2.39 mJy, respectively. b) The peak flux is $1.19\times 10^{-2}$ Jy. Contours drawn are -0.14, 0.14, 0.37, 0.63, 0.91, 1.35, 1.22, 1.56, 1.93, 2.34, 2.79, 3.29, 3.83, 4.46, 5.10, 5.82, 6.62, 7.50, 8.47, 9.54 and 10.71 mJy. The beam size in this uniform weighted map is $247 \times 151$ mas (PA $82\hbox {$^\circ $ }$ ) and the rms noise is 59 $\mu$ Jy. The integral intensities of C1a+b and C1c are 6.61 mJy and 14.73 mJy, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0866fig4.ps} \end{figure}$ Figure 4: The reconnection driven jet model of Hirose et al. (1997). The stellar magnetosphere truncates the accretion disk forming a magnetically neutral ring around the star. The jet forms as a result of a reconnection outflow from this X-line. The disk magnetic field is assumed to be parallel to the stellar dipole moment.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0866fig5.ps} \end{figure}$ Figure 5: Ejection of a plasmoid from the stellar magnetosphere. Enhanced accretion during the periastron passage pushes the disk toward the symmetry axis until the dipole field lines reconnect and the plasmoid is ejected from the magnetosphere. The disk magnetic field is assumed to be antiparallel to the stellar dipole moment.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0866fig6.ps} \end{figure}$ Figure 6: The positions of components relative to core between 1982.74 and 1999.78. We have combined the positions of the five-years period during the 80's. The positions of these epochs are taken from Kafatos et al. (1983) (A and B), Hollis et al. (1986) (C1 and C2), Kafatos et al. (1989) (A $\hbox {$^\prime $ }$ and B $\hbox {$^\prime $ }$ ) and LJ (D).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0866fig4.ps} \end{figure}$	Figure 4: The reconnection driven jet model of Hirose et al. (1997). The stellar magnetosphere truncates the accretion disk forming a magnetically neutral ring around the star. The jet forms as a result of a reconnection outflow from this X-line. The disk magnetic field is assumed to be parallel to the stellar dipole moment.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0866fig5.ps} \end{figure}$	Figure 5: Ejection of a plasmoid from the stellar magnetosphere. Enhanced accretion during the periastron passage pushes the disk toward the symmetry axis until the dipole field lines reconnect and the plasmoid is ejected from the magnetosphere. The disk magnetic field is assumed to be antiparallel to the stellar dipole moment.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0866fig6.ps} \end{figure}$	Figure 6: The positions of components relative to core between 1982.74 and 1999.78. We have combined the positions of the five-years period during the 80's. The positions of these epochs are taken from Kafatos et al. (1983) (A and B), Hollis et al. (1986) (C1 and C2), Kafatos et al. (1989) (A $\hbox {$^\prime $ }$ and B $\hbox {$^\prime $ }$ ) and LJ (D).
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