Study of the magnetoconvection and oscillations in the upper convection zone by means of realistic numerical simulations

Details Study of the magnetoconvection and oscillations in the upper convection zone by means of realistic numerical simulations Study of the magnetoconvection and oscillations in the upper convection zone by means of realistic numerical simulations

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp21a..06j&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SP21A-06

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy, 7524 Magnetic Fields, 7529 Photosphere

Scientific paper

Recent high-resolution data from the Hinode space mission have shown that magnetic fields on the Sun are concentrated in small high-intensity magnetic flux tubes in the intergranular lanes. Our objective is to investigate how magnetic field affects the dynamics of granular convection and excitation of solar oscillations by means of realistic numerical simulations. We have used a 3D, compressible, non-linear radiative magnetohydrodynamics code developed at the NASA Ames Research Center. This code takes into account several physical phenomena: compressible fluid flow in a highly stratified medium, sub-grid scale turbulence models, radiative energy transfer between the fluid elements, and a real-gas equation of state. We have studied the influence of the magnetic field of various strength on the convective cells and on the excitation mechanisms of the acoustic oscillations by calculating spectral properties of the convective motions and oscillations. The results reveal substantial changes of the granulation structure with increased magnetic field, and a frequency-dependent reduction in the oscillation power. The simulation results are compared with Hinode observations.

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