Astronomy and Astrophysics – Astronomy
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.2911p&link_type=abstract
American Astronomical Society Meeting 210, #29.11; Bulletin of the American Astronomical Society, Vol. 39, p.139
Astronomy and Astrophysics
Astronomy
Scientific paper
We developed a method to model the emission of some UV lines behind a coronal shock wave. This approach is designed to constrain the properties of the coronal atmosphere and the CME event when a shock is present. Several CME observations are related to shock waves propagating in the corona, but some questions remain about the properties of those shocks. In particular, the observed shock speed does not match that inferred from radio observations and the compression of the shocked plasma is quite weak. A full MHD 3-D model of the propagation of a supersonic dense fragment in the solar corona has been implemented to simulate the production of shocks during the CME events. In this context, we model both the evolution of the plasma and the magnetic field taking into account the solar gravity, the radiative losses and the thermal conduction in presence of a magnetic field. Solving the full MHD equations, we compute the intensity of several UVCS lines (O VI, Si XII, Lyman α and β from the coronal plasma thermodynamic properties as function of time inside the full domain. Non-equilibrium ionization effects are considered for the emission lines, since the actual ion abundances due to the lagrangian transport of ions and to the ionization/recombination processes are used to compute the collisional and radiative parts of the lines. This procedure allow us to predict the spectral observations with UVCS, and to explore the parameter space to investigate the properties of shocks related with CMEs. Finally, the 3-D approach will allow us also to consider the effect of the integration along the line of sight.
Pagano Paolo
Raymond John C.
Reale Fabio
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