Numerical Modeling of Transition Region Dynamics

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