  Double coronal hard X-ray (HXR) sources are believed to be critical
observational evidence of bi-directional energy release through magnetic
reconnection in a large-scale current sheet in solar ares. Here we present a
study on double coronal sources observed in both HXR and microwave regimes,
revealing new characteristics distinct from earlier reports. This event is
associated with a footpoint-occulted X1.3-class flare (25 April 2014, starting
at 00:17 UT) and a coronal mass ejection that are likely triggered by the
magnetic breakout process, with the lower source extending upward from the top
of the partially-occulted flare loops and the upper source co-incident with
rapidly squeezing-in side lobes (at a speed of ~250 km/s on both sides). The
upper source can be identified at energies as high as 70-100 keV. The X-ray
upper source is characterized by flux curves different from the lower source, a
weak energy dependence of projected centroid altitude above 20 keV, a shorter
duration and a HXR photon spectrum slightly-harder than those of the lower
source. In addition, the microwave emission at 34 GHz also exhibits a similar
double source structure and the microwave spectra at both sources are in line
with gyro-synchrotron emission given by non- thermal energetic electrons. These
observations, especially the co-incidence of the very-fast squeezing-in motion
of side lobes and the upper source, indicate that the upper source is
associated with (possibly caused by) this fast motion of arcades. This sheds
new lights on the origin of the corona double-source structure observed in both
HXRs and microwaves.
