  We have investigated a supra-arcade structure, associated with an M1.6 flare,
which occurred on the south-east limb on 4th of November 2010. It is observed
in microwaves at 17 GHz with the Nobeyama Radioheliograph (NoRH), soft X-rays
in the range of 8-20 keV with the Reuven Ramaty High Energy Solar Spectroscopic
Imager (RHESSI), and EUV with the Atmospheric Imaging Assembly (AIA) onboard
the Solar Dynamics Observatory (SDO). As reported by Reeves & Golub (2011), the
supra-arcade structure is observed predominantly in the AIA 131 {\AA} channel,
which contains a hot 11 MK component from Fe XIX (Boerner et al. 2011). While
this hot flare plasma lasts over the decay phase of the flare, it shows some
interesting characteristics in microwaves and soft X-rays: 1) In the
supra-arcade structure, the brightness temperature (TB) of the microwave
emission increases gradually up to 2\times10^4 K, and 2) two soft X-ray sources
appear: one cospatial with the supra-arcade structure and another above the
post-flare arcade. We have derived the variation of emission measure, density,
and energy of the supra-arcade structure using the TB obtained from 17 GHz
microwave observations.
