The analysis of the Parker–Moffatt problem, recently revisited in Pezzi
et al. (Astrophys. J., vol. 834,
2017, p. 166), is here extended by including Hall magnetohydrodynamics and two
hybrid kinetic Vlasov–Maxwell numerical models. The presence of dispersive and
kinetic features is studied in detail and a comparison between the two kinetic codes
is also reported. Focus on the presence of non-Maxwellian signatures shows that
– during the collision – regions characterized by strong temperature
anisotropy are recovered and the proton distribution function displays a beam along
the direction of the magnetic field, similar to some recent observations of the solar
wind.