Numerical Models of solar Magnetoconvection: Toward a Coupling to the Corona

Details Numerical Models of solar Magnetoconvection: Toward a Coupling to the Corona Numerical Models of solar Magnetoconvection: Toward a Coupling to the Corona

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...204.3908d&link_type=abstract

American Astronomical Society Meeting 204, #39.08; Bulletin of the American Astronomical Society, Vol. 36, p.715

Astronomy and Astrophysics

Astronomy

Scientific paper

We present numerical simulations of a stratified magnetized fluid, confined to a spherical shell, that approximates the transition from a high- to low-beta regime, similar to the conditions present at the solar photosphere. In these simulations, a model corona atmosphere is situated above a convectively unstable, high-beta fluid layer. As a result, the dynamics associated with evolving magnetic features in the solar atmosphere can be modeled in a manner that is self-consistent with the convective motions that provide the driving. Our simulations exhibit arcade-like structures that undergo reconnection as a result of the supergranular-scale fluid motions in the convective layer below, and discuss possible observational consequences.

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