Spectral Analysis of 3D MHD Models of Quiet Sun and Active Region Structures

Details Spectral Analysis of 3D MHD Models of Quiet Sun and Active Region Structures Spectral Analysis of 3D MHD Models of Quiet Sun and Active Region Structures

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...12.3.39z&link_type=abstract

"12th European Solar Physics Meeting, Freiburg, Germany, held September, 8-12, 2008. Online at http://espm.kis.uni-freiburg.de/,

Physics

Scientific paper

We study EUV emission line spectra derived from 3D MHD models of structures in the corona, in particular of an active region surrounded by a strong chromospheric network. The 3D MHD models account properly for the energy balance, especially for heat conduction and radiative losses. This allows us to reliably synthesize the profiles of EUV emission lines observable with current EUV spectrometers, e.g. SUMER/SOHO and EIS/Hinode. We investigate the temporal evolution and spatial distribution of the Doppler shifts of the EUV emission lines synthesized from these models. This is of major interest for the underlying mechanism of the heating of the solar corona, i.e. dissipation of currents in the corona driven by photospheric motions (flux braiding). Based on the 3D MHD models we can also derive intensity maps as they will be observed through the coronal channels of the AIA-instrument onboard SDO and we can analyze how to process the AIA maps in order to derive physical quantities such as temperatures and densities. Since we have access not only to the synthetic spectra, but also to the magnetic field in the box we can explore how the magnetic field relates to the emission in various coronal lines. In the present paper we will show results on the evolution of spectral properties such as line shifts or widths in different modeled coronal structures and compare these to results from SUMER/SOHO as well as EIS/Hinode data.

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