[41] In conclusion we briefly formulate the main results:
[42] 1. Temporal profile of hard X-ray emission related to the flare on 29 October 2002 manifests itself as a sequence of spikes with the duration 10-30 ms at half maximum of their amplitude, which is comparable to the minimal spike duration registered up to now in the radio frequency range.
[43] 2. In the registered flux of hard X-ray emission during the flare quasiperiodic component with the period 0.35 s appears. This component is absent in preflare or postflare radiation and which can be explained by "tearing-mode'' instability.
[44] 3. In hard X-ray emission of the flare oscillation with the period 3.5 s appears, while in soft X-ray emission, with the period 9.5 s, which can be explained by fast sausage MHD oscillations at the fundamental harmonic.
[45] 4. The energetic spectrum of the discussed flare can be divided
into two parts with the "inflection point''
45 KeV. The part of
the spectrum with the energies smaller than the inflection point
probably is produced by the thermal radiation of hot plasma, while
the high-energy part of spectrum above the inflection point is
explained by fast electrons bremsstrahlung.
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