High <b> <i>β</i> </b> magnetic reconnection at different altitudes in the cool low solar atmosphere

We numerically studied magnetic reconnection in a high β hydrogen–helium plasma at different altitudes from the photosphere to upper chromosphere. The time-dependent ionization degrees were included get more realistic diffusivities and viscosity, appropriate radiative cooling models applied. Our numerical results indicate that plasmoid instability always plays vital role speeding up atmospheric layers. In addition, both strong diffusion caused by electron–neutral collision (ηen) can significantly accelerate below middle On other hand, ambipolar viscosity result higher temperature pressure region chromosphere, which then hinders fast process developing. local compression heating triggered turbulent mediated with plasmoids is dominant mechanism unstable stage layers, but viscous are equally important Joule contributed ηen dominates during early quasi-steady also leads much stronger generation of thermal energy this region. Though same all simulation cases altitudes, increase significant chromosphere lower density weaker cooling.