  Dispersive Alfven waves (DAWs) offer, an alternative to magnetic
reconnection, opportunity to accelerate solar flare particles. We study the
effect of DAW polarisation, L-, R-, circular and elliptical, in different
regimes inertial and kinetic on the efficiency of particle acceleration. We use
2.5D PIC simulations to study how particles are accelerated when DAW, triggered
by a solar flare, propagates in transversely inhomogeneous plasma that mimics
solar coronal loop. (i) In inertial regime, fraction of accelerated electrons
(along the magnetic field), in density gradient regions is ~20% by the time
when DAW develops 3 wavelengths and is increasing to ~30% by the time DAW
develops 13 wavelengths. In all considered cases ions are heated in transverse
to the magnetic field direction and fraction of the heated particles is ~35%.
(ii) The case of R-circular, L- and R- elliptical polarisation DAWs, with the
electric field in the non-ignorable transverse direction exceeding several
times that of in the ignorable direction, produce more pronounced parallel
electron beams and transverse ion beams in the ignorable direction. In the
inertial regime such polarisations yield the fraction of accelerated electrons
~20%. In the kinetic regime this increases to ~35%. (iii) The parallel electric
field that is generated in the density inhomogeneity regions is independent of
m_i/m_e and exceeds the Dreicer value by 8 orders of magnitude. (iv) Electron
beam velocity has the phase velocity of the DAW. Thus electron acceleration is
via Landau damping of DAWs. For the Alfven speeds of 0.3c the considered
mechanism can accelerate electrons to energies circa 20 keV. (v) The increase
of mass ratio from m_i/m_e=16 to 73.44 increases the fraction of accelerated
electrons from 20% to 30-35% (depending on DAW polarisation). For the mass
ratio m_i/m_e=1836 the fraction of accelerated electrons would be >35%.
