Simulation of spectral effects with the use of two-dimensional magnetohydrodynamic models of the solar photosphere.

Details Simulation of spectral effects with the use of two-dimensional magnetohydrodynamic models of the solar photosphere. Simulation of spectral effects with the use of two-dimensional magnetohydrodynamic models of the solar photosphere.

Jan 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996kpcb...12...24a&link_type=abstract

Kinematics Phys. Celest. Bodies, Vol. 12, No. 5, p. 24 - 35

Physics

2

Solar Photosphere: Magnetohydrodynamics, Solar Spectrum: Magnetohydrodynamics, Solar Spectrum: Numerical Simulations

Scientific paper

To study the structure of spatially unresolved features on the Sun, the authors calculated the Stokes profiles of seven photospheric iron lines using two-dimensional nonstationary MHD models of solar granulation for various amounts of magnetic flux. The authors investigate variations in the calculated absolute wavelength shifts and I-profile bisectors, zero-crossing wavelength shifts, amplitude asymmetry parameters, and V-profile areas as functions of magnetic field strength and time. The center-to-limb variations of the Stokes profiles are analyzed. The iron abundance is found to be 7.57, with the photosphere inhomogeneities taken into account. Although most of the spectral effects simulated within the scope of two-dimensional models are in satisfactory agreement with observational data, the two-dimensional approximation cannot always give a quantitative agreement. The absolute wavelength shifts calculated for Fe II lines are substantially smaller than the observed ones.

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