Numerical Simulations of Bipolar Magnetic Field Decay in Turbulent Convection

Details Numerical Simulations of Bipolar Magnetic Field Decay in Turbulent Convection Numerical Simulations of Bipolar Magnetic Field Decay in Turbulent Convection

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp11c..02d&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SP11C-02

Astronomy and Astrophysics

Astrophysics

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

Scientific paper

We present numerical simulations of compressible magnetoconvection in spherical segments, seeking to examine the decay of active region magnetic fields on the sun. It is surprising that after their emergence, active regions are observed to persist in relative stasis for long periods of time (weeks to months) before suddenly disintegrating. We perform a series of calculations to investigate this process, in which we drive turbulent convection (Rayleigh numbers of order 107) within two- and three-dimensional spherical segments, and measure the decay rates of the embedded bipolar magnetic fields.

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