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NUMERICAL MODELLING OF TRANSITION REGION L. TERIACA AND J. G. DOYLE
 

Summary: NUMERICAL MODELLING OF TRANSITION REGION
DYNAMICS
L. TERIACA AND J. G. DOYLE
Armagh Observatory
Armagh BT61 9DG, N. Ireland
Abstract. We explore the idea that the occurrence of nano­flares in a
magnetic loop around the O vi formation temperature could explain the
observed red­shift of mid­low transition region lines as well as the blue­shift
observed in low coronal lines (T ? 6 \Theta 10 5 K). Observations are compared to
numerical simulations of the response of the solar atmosphere to an energy
perturbation of 4 \Theta 10 24 ergs representing an energy release during magnetic
reconnection in a 1­D semi­circular 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 1:7km s \Gamma1 , are found in C iii, C iv, and
O v while blue­shifts of \Gamma1:8, \Gamma3:9 and \Gamma10:7 km s \Gamma1 were derived for O vi,
Ne vii and Ne viii respectively, in good agreement with observations.
1. Introduction
During the last two decades, observations of red­shifted emission lines

  

Source: Armagh Observatory

 

Collections: Physics