  We present results revealing microwave pulsations produced in a model of a
flaring twisted solar coronal loop, without any external oscillatory driver.
Two types of oscillations are identified: slowly-decaying oscillations with a
period of about 70-75s and amplitude of about 5-10% seen in loops both with and
without energetic electrons, and oscillations with period of about 40s and
amplitude of a few tens of percent observed only in loops with energetic
electrons for about 100s after onset of fast energy release. We interpret the
longer-period oscillations as the result of a standing kink mode modulating the
average magnetic field strength in the loop, whilst the short-period
intermittent oscillations associated with energetic electrons are likely to be
produced by fast variations of the electric field which produces energetic
electrons in this scenario. The slowly-decaying oscillations can explain the
quasi-periodic pulsations often observed in the flaring corona.
