All Figures

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{4816f1.eps}\end{figure}$ Figure 1: Dimensionless density (Eq. (1)), solid line, and Alfvén speed, dashed line, profiles across the uniform unperturbed magnetic field (i.e. along x-coordinate) which is used as an equilibrium configuration in our model of a footpoint of a solar coronal loop or a polar region plume.
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In the text

$\begin{figure} \par\includegraphics[width=5.7cm,clip]{4816f2a.eps}\hspace*{5mm} ... ...c.eps}\hspace*{5mm} \includegraphics[width=5.7cm,clip]{4816f2d.eps} \end{figure}$ Figure 2: Intensity plots of V_x and E_z at t=2 and 20 for the case of k=1, $\nu = 0.7$ Hz, $\lambda _{\rm A} = 6.3$ Mm.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4816f3.eps}\end{figure}$ Figure 3: Time evolution of the amplitudes of $V_x \equiv V_x^a$ and $E_z\equiv E_z^a$ . Solid lines represent solutions using the linear McCormack code, while dash-dotted lines with open symbols are the solutions using the non-linear code Lare2d. Here A=0.05, k=1, $\nu = 0.7$ Hz, $\lambda _{\rm A} = 6.3$ Mm, and both runs have 2000 $\times$ 2000 spatial grid resolution.
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In the text

$\begin{figure} \par\includegraphics[width=4.8cm,clip]{4816f4a.eps}\hspace*{1.3cm... ...ps}\hspace*{1.3cm} \includegraphics[width=4.95cm,clip]{4816f4d.eps} \end{figure}$ Figure 4: Snapshots of V_x and E_z at t=2 and 20 for the case of k=10, ${\nu = 7}$ Hz, $\lambda _{\rm A} = 0.63$ Mm.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4816f5.eps}\end{figure}$ Figure 5: Time evolution of the amplitudes of $V_x \equiv V_x^a$ and $E_z\equiv E_z^a$ . Solid lines with stars represent solutions using the Lare2d code with 4000 $\times$ 4000 resolution, while dash-dotted lines with open symbols are the same but with 2000 $\times$ 2000 resolution. Here A=0.05, k=10, ${\nu = 7}$ Hz, $\lambda _{\rm A} = 0.63$ Mm.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4816f6.eps}\end{figure}$ Figure 6: Time evolution of E_z at a point (x=10.68,z=0). Here k=1, $\nu = 0.7$ Hz, and $\lambda _{\rm A} = 6.3$ Mm.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4816f7.eps}\end{figure}$ Figure 7: Plot of the flux carried by Alfvén waves from 10^-4 Hz up to a frequency $\nu$ versus that frequency as inferred from the empirically constrained spectrum of Cranmer et al. (1999). The solid line corresponds to Eq. (18), while the dashed line shows te coronal heating requirement for a temperature of 1 MK.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{4816f1.eps}\end{figure}$	Figure 1: Dimensionless density (Eq. (1)), solid line, and Alfvén speed, dashed line, profiles across the uniform unperturbed magnetic field (i.e. along x-coordinate) which is used as an equilibrium configuration in our model of a footpoint of a solar coronal loop or a polar region plume.
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$\begin{figure} \par\includegraphics[width=5.7cm,clip]{4816f2a.eps}\hspace{5mm} ... ...c.eps}\hspace{5mm} \includegraphics[width=5.7cm,clip]{4816f2d.eps} \end{figure}$	Figure 2: Intensity plots of V_x and E_z at t=2 and 20 for the case of k=1, $\nu = 0.7$ Hz, $\lambda _{\rm A} = 6.3$ Mm.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4816f3.eps}\end{figure}$	Figure 3: Time evolution of the amplitudes of $V_x \equiv V_x^a$ and $E_z\equiv E_z^a$ . Solid lines represent solutions using the linear McCormack code, while dash-dotted lines with open symbols are the solutions using the non-linear code Lare2d. Here A=0.05, k=1, $\nu = 0.7$ Hz, $\lambda _{\rm A} = 6.3$ Mm, and both runs have 2000 $\times$ 2000 spatial grid resolution.
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$\begin{figure} \par\includegraphics[width=4.8cm,clip]{4816f4a.eps}\hspace{1.3cm... ...ps}\hspace{1.3cm} \includegraphics[width=4.95cm,clip]{4816f4d.eps} \end{figure}$	Figure 4: Snapshots of V_x and E_z at t=2 and 20 for the case of k=10, ${\nu = 7}$ Hz, $\lambda _{\rm A} = 0.63$ Mm.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4816f5.eps}\end{figure}$	Figure 5: Time evolution of the amplitudes of $V_x \equiv V_x^a$ and $E_z\equiv E_z^a$ . Solid lines with stars represent solutions using the Lare2d code with 4000 $\times$ 4000 resolution, while dash-dotted lines with open symbols are the same but with 2000 $\times$ 2000 resolution. Here A=0.05, k=10, ${\nu = 7}$ Hz, $\lambda _{\rm A} = 0.63$ Mm.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4816f6.eps}\end{figure}$	Figure 6: Time evolution of E_z at a point (x=10.68,z=0). Here k=1, $\nu = 0.7$ Hz, and $\lambda _{\rm A} = 6.3$ Mm.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4816f7.eps}\end{figure}$	Figure 7: Plot of the flux carried by Alfvén waves from 10^-4 Hz up to a frequency $\nu$ versus that frequency as inferred from the empirically constrained spectrum of Cranmer et al. (1999). The solid line corresponds to Eq. (18), while the dashed line shows te coronal heating requirement for a temperature of 1 MK.
Open with DEXTER