Effect of coronal temperature on the scale of solar chromospheric jets

Abstract

We investigate the effect of coronal temperature on the formation process of solar chromospheric jets using two-dimensional magnetohydrodynamic simulations of the region from the upper convection zone to the lower corona. We develop a new radiative magnetohydrodynamic code for the dynamic modeling of the solar atmosphere, employing a LTE equation of state, optically thick radiative loss in the photosphere, optically thin radiative loss in the chromosphere and the corona, and thermal conduction along the magnetic field lines. Many chromospheric jets are produced in the simulations by shock waves passing through the transition region. We find that these jets are projected farther outward when the coronal temperature is lower (similar to that in coronal holes) and shorter when the coronal temperature is higher (similar to that in active regions). When the coronal temperature is high, the deceleration of the chromospheric jets is consistent with the model in which deceleration is determined by the periodic chromospheric shock waves. However, when the coronal temperature is low, the gravitational deceleration becomes more important and the chromospheric jets approach ballistic motion.

19 pages, 4 figures, accepted for publication in ApJL

References in corpus (9)

• Observing the Roots of Solar Coronal Heating - in the Chromosphere
• Dynamic Fibrils are driven by Magnetoacoustic Shocks
• High Resolution Observations and Modeling of Dynamic Fibrils
• Preserving Monotonicity in Anisotropic Diffusion
• An Interface Region Imaging Spectrograph first view on Solar Spicules
• Magnetoacoustic shocks as driver of quiet Sun mottles
• Revision of Solar Spicule Classification
• Observational Signatures of Simulated Reconnection Events in the Solar Chromosphere and Transition Region
• Radiating Current Sheets in the Solar Chromosphere

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