Numerical Modeling of the Transition Region Dynamics

Details Numerical Modeling of the Transition Region Dynamics Numerical Modeling of the Transition Region Dynamics

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001assl..259..307t&link_type=abstract

The Dynamic Sun, Proceedings of the Summerschool and Workshop held at the Solar Observatory Kanzelhöhe, Kärnten, Austria, August

Astronomy and Astrophysics

Astrophysics

2

Scientific paper

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 times 105 K). Observations are compared to numerical simulations of the response of the solar atmosphere to an energy perturbation of 4 times 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 O 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.

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