Realistic numerical simulations of solar convection and oscillations in magnetic regions

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

doi:10.1086/592042

Realistic numerical simulations of solar convection and oscillations in magnetic regions

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

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55 Scopus citations

Abstract

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 language	English (US)
Pages (from-to)	L51-L54
Journal	Astrophysical Journal
Volume	684
Issue number	1
DOIs	https://doi.org/10.1086/592042
State	Published - Sep 1 2008
Externally published	Yes

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Convection
Methods: numerical
Sun: oscillations

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10.1086/592042

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abstract = "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.",

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T1 - Realistic numerical simulations of solar convection and oscillations in magnetic regions

AU - Jacoutot, L.

AU - Kosovichev, A. G.

AU - Wray, A.

AU - Mansour, N. N.

PY - 2008/9/1

Y1 - 2008/9/1

N2 - 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.

AB - 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.

KW - Convection

KW - Methods: numerical

KW - Sun: oscillations

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JF - Astrophysical Journal

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Realistic numerical simulations of solar convection and oscillations in magnetic regions

Abstract

All Science Journal Classification (ASJC) codes

Keywords

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