Realistic numerical simulations of solar convection and oscillations in magnetic regions

L. Jacoutot, A. G. Kosovichev, A. Wray, N. N. Mansour

Research output: Contribution to journalArticlepeer-review

55 Scopus citations


We have used 3D, compressible, nonlinear radiative magnetohydrodynamics simulation to study the influence of magnetic fields of various strengths on convective cells and on the excitation mechanisms of acoustic oscillations by calculating the 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 in a good agreement with solar observations. These simulations suggest that the enhanced high-frequency acoustic emission at the boundaries of active regions ("acoustic halo" phenomenon) is caused by changes of the spatial-temporal spectrum of turbulent convection in a magnetic field, resulting in turbulent motions of smaller scales and higher frequencies than in quiet-Sun regions.

Original languageEnglish (US)
Pages (from-to)L51-L54
JournalAstrophysical Journal
Issue number1
StatePublished - Sep 1 2008
Externally publishedYes

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science


  • Convection
  • Methods: numerical
  • Sun: oscillations


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