  We present data analysis and interpretation of an M1.4-class flare observed
with the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) on April
30, 2002. This event, with its footpoints occulted by the solar limb, exhibits
a rarely observed, but theoretically expected, double-source structure in the
corona. The two coronal sources, observed over the 6-30 keV range, appear at
different altitudes and show energy-dependent structures with the higher-energy
emission being closer together. Spectral analysis implies that the emission at
higher energies in the inner region between the two sources is mainly
nonthermal, while the emission at lower energies in the outer region is
primarily thermal. The two sources are both visible for about 12 minutes and
have similar light curves and power-law spectra above about 20 keV. These
observations suggest that the magnetic reconnection site lies between the two
sources. Bi-directional outflows of the released energy in the form of
turbulence and/or particles from the reconnection site can be the source of the
observed radiation. The spatially resolved thermal emission below about 15 keV,
on the other hand, indicates that the lower source has a larger emission
measure but a lower temperature than the upper source. This is likely the
result of the differences in the magnetic field and plasma density of the two
sources.
