  We analyze a confined flare that developed a hot cusp-like structure high in
the corona (H ~ 66 Mm). A growing cusp-shaped flare arcade is a typical feature
in the standard model of eruptive flares, caused by magnetic reconnection at
progressively larger coronal heights. In contrast, we observe a static hot cusp
during a confined flare. Despite an initial vertical temperature distribution
similar to that in eruptive flares, we observe a distinctly different evolution
during the late (decay) phase, in the form of prolonged hot emission. The
distinct cusp shape, rooted at locations of non-thermal precursor activity, was
likely caused by a magnetic field arcade that kinked near the top. Our
observations indicate that the prolonged heating was a result of slow local
reconnection and an increased thermal pressure near the kinked apexes due to
continuous plasma upflows.
