  A popular scenario for electron acceleration in solar flares is transit-time
damping of low-frequency MHD waves excited by reconnection and its outflows.
The scenario requires several processes in sequence to yield energetic
electrons of the observed large number. Until now there was very little
evidence for this scenario, as it is even not clear where the flare energy is
released. RHESSI measurements of bremsstrahlung by non-thermal flare electrons
yield energy estimates as well as the position where the energy is deposited.
Thus quantitative measurements can be put into the frame of the global magnetic
field configuration as seen in coronal EUV line observations. We present RHESSI
observations combined with TRACE data that suggest primary energy inputs mostly
into electron acceleration and to a minor fraction into coronal heating and
primary motion. The more sensitive and lower energy X-ray observations by
RHESSI have found also small events (C class) at the time of the acceleration
of electron beams exciting meter wave Type III bursts. However, not all RHESSI
flares involve Type III radio emissions. The association of other decimeter
radio emissions, such as narrowband spikes and pulsations, with X-rays is
summarized in view of electron acceleration
