$\begin{figure} \par\includegraphics[width=7cm,clip]{NEWfigs/2499fig1.eps} \end{figure}$ Figure 1: The growth rates, $\gamma _* = \gamma +\eta k^2$ in units of ${A}=q\Omega /2$ as functions of the normalized field strength for MRI alone (full line) and MRI modified by the Hall effect of positive fields ( $\beta = 1$ , dashed line) and negative fields ( $\beta = -1$ , dashed-dotted). ${\rm Pm} =1$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=6cm,width=7cm,clip]{NEWfigs/2499fig2.eps} \end{figure}$ Figure 2: Neutral stability lines of the MRI for various magnetic Prandtl numbers ( $C_{\rm H}=0$ ). For ${\rm Pm} < 0.1$ the lines are almost independent of Pm.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=6cm,width=7cm,clip]{NEWfigs/2499fig3.eps} \end{figure}$ Figure 3: Stability diagram for the shear-Hall instability (positive magnetic field, i.e. parallel to the rotation axis; only the induction equation is solved). Lines are labeled by their symmetry types. The axisymmetric quadrupolar mode (S0) is preferred.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{ \includegraphics[width=4.3truecm]{NEWfigs/2499fig4a.eps} \includegraphics[width=4.3truecm]{NEWfigs/2499fig4b.eps} } \end{figure}$ Figure 4: Magnetic field vectors in the disk midplane for marginally stable S0-modes at ${\rm Rm}=100$ for the minimum ( left) and maximum ( right) Lundquist numbers, resp. The broken circle shows the turnover radius R₀ of the rotation law.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=6cm,width=7cm,clip]{NEWfigs/2499fig5.eps} \end{figure}$ Figure 5: The same as in Fig. 3 but for the full equation system. The Hall effect increases the minimum Rm. The solid curve for $\beta \to \infty$ is identical to the lower curve in Fig. 3. For increasing Rm the lower limit for the magnetic field becomes smaller and smaller.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=6cm,width=7cm,clip]{NEWfigs/2499fig6.eps} \end{figure}$ Figure 6: Stability diagram for MRI modified by the Hall effect for magnetic fields antiparallel to the angular velocity. Note that the Hall parameter $\beta$ for real cool protostellar disks is of order unity. The Hall effect shifts the instability interval to larger Lundquist numbers, i.e. to higher magnetic fields.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=7.2cm,width=8.5cm,clip]{NEWfigs/2499fig7.eps} \end{figure}$ Figure 7: The computed minimum magnetic Reynolds number as a function of the Hall parameter. $\beta =0$ denotes MRI. The results for $\beta <-0.3$ are not yet known.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{NEWfigs/2499fig1.eps} \end{figure}$	Figure 1: The growth rates, $\gamma _* = \gamma +\eta k^2$ in units of ${A}=q\Omega /2$ as functions of the normalized field strength for MRI alone (full line) and MRI modified by the Hall effect of positive fields ( $\beta = 1$ , dashed line) and negative fields ( $\beta = -1$ , dashed-dotted). ${\rm Pm} =1$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[height=6cm,width=7cm,clip]{NEWfigs/2499fig2.eps} \end{figure}$	Figure 2: Neutral stability lines of the MRI for various magnetic Prandtl numbers ( $C_{\rm H}=0$ ). For ${\rm Pm} < 0.1$ the lines are almost independent of Pm.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=6cm,width=7cm,clip]{NEWfigs/2499fig3.eps} \end{figure}$	Figure 3: Stability diagram for the shear-Hall instability (positive magnetic field, i.e. parallel to the rotation axis; only the induction equation is solved). Lines are labeled by their symmetry types. The axisymmetric quadrupolar mode (S0) is preferred.
Open with DEXTER

$\begin{figure} \par\mbox{ \includegraphics[width=4.3truecm]{NEWfigs/2499fig4a.eps} \includegraphics[width=4.3truecm]{NEWfigs/2499fig4b.eps} } \end{figure}$	Figure 4: Magnetic field vectors in the disk midplane for marginally stable S0-modes at ${\rm Rm}=100$ for the minimum ( left) and maximum ( right) Lundquist numbers, resp. The broken circle shows the turnover radius R₀ of the rotation law.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=6cm,width=7cm,clip]{NEWfigs/2499fig5.eps} \end{figure}$	Figure 5: The same as in Fig. 3 but for the full equation system. The Hall effect increases the minimum Rm. The solid curve for $\beta \to \infty$ is identical to the lower curve in Fig. 3. For increasing Rm the lower limit for the magnetic field becomes smaller and smaller.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=6cm,width=7cm,clip]{NEWfigs/2499fig6.eps} \end{figure}$	Figure 6: Stability diagram for MRI modified by the Hall effect for magnetic fields antiparallel to the angular velocity. Note that the Hall parameter $\beta$ for real cool protostellar disks is of order unity. The Hall effect shifts the instability interval to larger Lundquist numbers, i.e. to higher magnetic fields.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=7.2cm,width=8.5cm,clip]{NEWfigs/2499fig7.eps} \end{figure}$	Figure 7: The computed minimum magnetic Reynolds number as a function of the Hall parameter. $\beta =0$ denotes MRI. The results for $\beta <-0.3$ are not yet known.
Open with DEXTER