The boundary integral equation for non-force-free field modelling in solar atmosphere

Details The boundary integral equation for non-force-free field modelling in solar atmosphere The boundary integral equation for non-force-free field modelling in solar atmosphere

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.506..401y&link_type=abstract

In: Solar variability: from core to outer frontiers. The 10th European Solar Physics Meeting, 9 - 14 September 2002, Prague, Cze

Physics

1

Sun: Magnetic Field, Sun: Corona, Sun: Activity, Mhd

Scientific paper

The plasma β is much less than one in the corona and a force-free field model is a good approximation there. However, at photosphere the low-β condition is no longer valid but the reliable magnetic field measurements are confined to the photosphere, which are normally used as the boundary condition for the extrapolation upwards in the force-free field model. Low (1992) has provided a non-force-free field model based on the magnetostatic equilibrium, and applications to observations have been done but with linear model. Here we apply the boundary element method that has been employed for non-constant-α force-free field (Yan and Sakurai 1997, 2000) to the non-force-free field model, and discuss the influence of the boundary data to the reconstructed field in the corona.

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