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Numerical Modeling of Transition Region Dynamics

  • L. Teriaca
  • J. G. Doyle
Conference paper
Part of the Astrophysics and Space Science Library book series (ASSL, volume 259)

Abstract

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.

Keywords

Transition Region Line Profile Magnetic Reconnect Solar Atmosphere Magnetic Loop 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer Science+Business Media Dordrecht 2001

Authors and Affiliations

  • L. Teriaca
    • 1
  • J. G. Doyle
    • 1
  1. 1.Armagh ObservatoryArmaghN. Ireland

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