H-alpha (left column) and TRACE/EUV (right column) observations
prior to and after a filament eruption on 2008 May 16.
(a) Magnetic map of the decaying active region on 2008 May 16 at 11:42 UT
derived from THEMIS and SOHO/MDI data. (b) and (c) Zoomed regions enclosed
by white and black boxes in (a). The grayscale images in each panel show the radial
magnetic field Br in the photosphere as function of longitude and latitude
on the Sun. In panels (a) and (d), the white lines ending with two circles refer to the
selected filament paths along which flux ropes are inserted.
NLFFF models on May 16 at 11:42 UT (first row) and May 17 at 08:03 UT (second row).
The red and green contours refer to positive and negative magnetic fields from THEMIS+MDI
(first row) and MDI (second row). The red lines in the first column refer to selected
coronal loops observe by TRACE or XRT. The pink, blue, and light blue lines are the best-fit
model field lines. Dips of model field lines (yellow) are shown in the second column.
Quasi Separatrix Layer (QSL) maps at height of 1 Mm for different models.
(a) NLFFF model at 11:42 UT on 2008 May 16. (b)--(d) Potential field model,
NLFFF model with two flux ropes, and NLFFF model with three flux ropes at 08:03 UT
on 2008 May 17. The open field region is indicated in yellow, while the field lines
in the blue area are closed. The white layers are the quasi separatrix layers.
Front (first column) and side (second column) views of NLFFF models with selected
field lines on May 16 at 11:42 UT (first row) and May 17 at 08:03 UT (second row).
Vectors in small zoomed regions from the potential field model (first row) and the best-fit
NLFFF model (second row) at 11:42 UT on 2008 May 16. The maximum horizontal
field strength in unit of Gauss is shown at the lower right corner of each panel.
