Numerical simulations of the Sun's photospheric magnetic network and its evolution over the solar cycle

Details Numerical simulations of the Sun's photospheric magnetic network and its evolution over the solar cycle Numerical simulations of the Sun's photospheric magnetic network and its evolution over the solar cycle

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh43b1942t&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH43B-1942

Astronomy and Astrophysics

Astrophysics

[7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7529] Solar Physics, Astrophysics, And Astronomy / Photosphere, [7536] Solar Physics, Astrophysics, And Astronomy / Solar Activity Cycle

Scientific paper

We model, through 2D Monte-Carlo simulations on a spherical shell, the spatiotemporal evolution of the photospheric magnetic network over solar cycle timescales. Sources of magnetic flux in the simulations include both injection of small-scale magnetic structures all over the quiet sun, as well as the emergence and subsequent disintegration of sunspots in active latitudes. We simulate the emergence, random walk, interaction (aggregation or cancellation) and submergence of the smallest magnetic elements and aggregates thereof, also taking into account advection by differential rotation and meridional circulation. Although magnetic flux is injected only at the two extreme ends of the flux scale (elementary flux tubes and sunspots), the simulations produce a range of intermediate scales through aggregation and cancellation of the small-scale magnetic structures, whether injected all over the solar surface (Quiet Sun) or re- leased by the decaying sunspots. Moreover, the modeled flux is distributed in the form of a power law, as observed by Parnell et al. (2009). We in- vestigate how this distribution varies as a function fo solar cycle phase.

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