Numerical Modeling of Transition Region Dynamics
We explore the idea that the occurrence of nano-flares in a magnetic loop around the O VI formation temperature could explain the observed red-shift of mid-low transition region lines as well as the blue-shift observed in low coronal lines (T > 6 × 105 K). Observations are compared to numerical simulations of the response of the solar atmosphere to an energy perturbation of 4 × 1024 ergs representing an energy release during magnetic reconnection in a 1-D semi-circular flux tube. The temporal evolution of the thermodynamic state of the loop is finally converted into C III 977, C IV 1548, O V 630, O VI 1032, Ne VII 465 and Ne VIII 770 line profiles in non-equilibrium ionization. Performing an integration over the entire period of simulation, redshifts of 8.5, 6.1 and 1.7 km s−1, are found in C III, C IV, and 0 V while blue-shifts of −1.8, −3.9 and −10.7 km s−1 were derived for O VI, Ne VII and Ne VIII respectively, in good agreement with observations.
KeywordsTransition Region Line Profile Magnetic Reconnect Solar Atmosphere Magnetic Loop
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