Dynamical Interaction of Solar Magnetic Elements and Granular Convection: Results of a Numerical Simulation

Details Dynamical Interaction of Solar Magnetic Elements and Granular Convection: Results of a Numerical Simulation Dynamical Interaction of Solar Magnetic Elements and Granular Convection: Results of a Numerical Simulation

Mar 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...495..468s&link_type=abstract

Astrophysical Journal v.495, p.468

Astronomy and Astrophysics

Astronomy

135

Polarization, Radiative Transfer, Shock Waves, Sun: Granulation, Sun: Magnetic Fields, Convection

Scientific paper

Nonstationary convection in the solar photosphere and its interaction with photospheric magnetic structures (flux sheets in intergranular lanes) have been simulated using a numerical code for two-dimensional MHD with radiative energy transfer. Dynamical phenomena are identified in the simulations, which may contribute to chromospheric and coronal heating. Among these are the bending and horizontal displacement of a flux sheet by convective flows and the excitation and propagation of shock waves both within and outside the magnetic structure. Observational signatures of these phenomena are derived from calculated Stokes profiles of Zeeman-sensitive spectral lines. We suggest that the extended red wings of the observed Stokes V profiles are due to downward coacceleration of magnetized material in a turbulent boundary layer between the flux sheet and the strong external downflow. Upward-propagating shocks in magnetic structures should be detectable if a time resolution of about 10 s is achieved, together with a spatial resolution that allows one to isolate individual magnetic structures. Determination of the complicated internal dynamics of magnetic elements requires observations with a spatial resolution better than 100 km in the solar photosphere.

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