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$\begin{figure} \par\includegraphics[width=17cm,clip]{fig1.eps}\end{figure}$ Figure 1: Resonance diagram of the decay instability: resonant perpendicular wavenumber $X=k_{x}\lambda _{\rm D}$ vs. parallel wavenumbers $Z=k_{z}\lambda _{\rm D}$ of the resonant Langmuir waves. Parameter $b=\Omega _{\rm e}/\omega _{\rm pe}=1.04$ (solid line); 1.1(dash line), and 1.4 (dot line). The electron thermal velocity $V_{T{\rm e}}/c=1/70$ .
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{fig2.eps} \end{figure}$ Figure 2: Nonlinear growth rate of the decay L $\rightleftarrows$ KAW + W for Langmuir waves excited in the solar corona by electron beams. For the beam-driven Langmuir waves, the values of the dispersive variable $% Z=k_{{\rm L}z}\lambda _{\rm D}=0.01{-}0.04$ are taken for the spectrum of waves excited by the electron beams with respective velocities $V_{\rm b}/c=1/3$ -1/4. The normalized Langmuir wave energy is $W_{\rm L}=10^{-4}$ . Parameter $b=\Omega _{\rm e}/\omega _{\rm pe}=1.04$ (solid line); 1.1 (dash line), and 1.4 (dot line). The electron thermal velocity $V_{T{\rm e}}/c=1/70$ .
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{fig1.eps}\end{figure}$	Figure 1: Resonance diagram of the decay instability: resonant perpendicular wavenumber $X=k_{x}\lambda _{\rm D}$ vs. parallel wavenumbers $Z=k_{z}\lambda _{\rm D}$ of the resonant Langmuir waves. Parameter $b=\Omega _{\rm e}/\omega _{\rm pe}=1.04$ (solid line); 1.1(dash line), and 1.4 (dot line). The electron thermal velocity $V_{T{\rm e}}/c=1/70$ .
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