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In this paper we investigate, by means of two-dimensional magnetohydrodynamicsimulations, the impact of temperature-dependent resistivity and thermalconduction on the development of plasmoid instabilities in reconnecting currentsheets in the solar corona. We find that the plasma temperature in the currentsheet region increases with time and it becomes greater than that in the inflowregion. As secondary magnetic islands appear, the highest temperature is notalways found at the reconnection $X$-points, but also inside the secondaryislands. One of the effects of anisotropic thermal conduction is to decreasethe temperature of the reconnecting $X-$points and transfer the heat into the$O-$points, the plasmoids, where it gets trapped. In the cases withtemperature-dependent magnetic diffusivity, $\eta \sim T^{-3/2}$, the decreasein plasma temperature at the $X-$points leads to: (i) increase in the magneticdiffusivity until the characteristic time for magnetic diffusion becomescomparable to that of thermal conduction; (ii) increase in the reconnectionrate; and, (iii) more efficient conversion of magnetic energy into thermalenergy and kinetic energy of bulk motions. These results provide furtherexplanation of the rapid release of magnetic energy into heat and kineticenergy seen during flares and coronal mass ejections. In this work, wedemonstrate that the consideration of anisotropic thermal conduction andSpitzer-type, temperature-dependent magnetic diffusivity, as in the real solarcorona, are crucially important for explaining the occurrence of fastreconnection during solar eruptions.

Impact of Temperature-dependent resistivity and thermal conduction on plasmoid Instabilities in current sheets in the solar corona