  From 2014 October 19 to 27, six X-class flares occurred in super active
region (AR) 12192. They were all confined flares and were not followed by
coronal mass ejections (CMEs). To examine the structures of the four flares
close to the solar disk center from October 22 to 26, we employ firstly
composite triple-time images in each flare process to display {the stratified
structure} of these flare loops. The loop structures of each flare in both
lower (171 {\AA}) and higher (131 {\AA}) temperature channels are complex,
e.g., the flare loops rooting at flare ribbons are sheared or twisted (enwound)
together, and the complex structures have not been destroyed during the flares.
For the first flare, although the flare loop system appears as a spindle shape,
we can estimate their structure from observations, with lengths ranging from
130 to 300 Mm, heights from 65 to 150 Mm, widths at the middle part of the
spindle from 40 to 100 Mm, and shear angles from 16$^\circ$ to 90$^\circ$.
Moreover, the flare ribbons display irregular movements, such as the left
ribbon fragments of the flare on 22 swept a small region repeatedly, and the
both ribbons of the flare on 26 moved along the same direction, instead of
separating from each other. These irregular movements also imply that the
corresponding flare loops are complex, e.g. several sets of flare loops are
twisted together. Although previous studies suggest that the background
magnetic fields prevent confined flares from erupting, we firstly suggest based
on these observations that the complex flare loop structures may be responsible
for these confined flares.
