  Temporal and spectral characteristics of X-ray emission from 60 flares of
intensity $\ge$C class observed by Solar X-ray Spectrometer (SOXS) during
2003-2011 are presented. We analyse the X-ray emission observed in four and
three energy bands by the Si and CZT detectors, respectively. The number of
peaks in the intensity profile of the flares varies between 1 and 3. We find
moderate correlation (R$\simeq$0.2) between the rise time and the peak flux of
the first peak of the flare irrespective to energy band, which is indicative of
its energy-independent nature. Moreover, magnetic field complexity of the
flaring region is found to be anti-correlated (R=0.61) with the rise time of
the flares while positively correlated (R=0.28) with the peak flux of the
flare. The time delay between the peak of the X-ray emission in a given energy
band and that in the 25-30 keV decreases with increasing energy suggesting
conduction cooling to be dominant in the lower energies. Analysis of 340
spectra from 14 flares reveals that the peak of Differential Emission Measure
(DEM) evolution delays by 60-360 s relative to that of the temperature, and
this time delay is inversely proportional to the peak flux of the flare. We
conclude that temporal and intensity characteristics of flares are energy
dependent as well as magnetic field configuration of the active region.
