The effect of the coronal temperature on the formation process of the solar chromospheric jet is investigated using the two-dimensional radiation magnetohydrodynamic simulations. The high resolution observation by the Hinode satellite revealed various characteristics of the solar chromospheric jets like the spicules and the active region dynamic fibrils. However, the physical mechanism of the spicule is still under debate.
In this study, we present the results of the two-dimensional simulations including the upper convection zone to the lower corona to investigate the effect of the coronal temperature on the formation process of the solar chromospheric jet. We newly develop a radiative magnetohydrodynamic code for the dynamic modeling of the solar atmosphere, which includes the realistic equation of states, the optically thick radiative loss in the convection zone and the photosphere, the optically thin radiative loss in the chromosphere and the corona, and the anisotropic thermal conduction by the non-thermal electron.
Many chromospheric jets are produced in the simulation by the shock waves passing through the transition region. These jets become taller when the coronal temperature is low like the coronal hole, and shorter when the coronal temperature is high like the active region. In this presentation, we will report the quantitative analysis of the difference and discuss the physical mechanism of the dependence.