We have recently explored mass ejection from neutron star-torus systems formed after binary neutron star mergers of relatively low total mass in viscous and resistive MHD simulations in general relativity. The mass, velocity, and electron fraction of the ejecta are studied. We show that the r-process nucleosynthesis elemental pattern is not very likely to agree with the solar abundance one, and hence, this type of the binary neutron stars may be a minority. Also MHD numerical relativity simulations show that the ejecta kinetic energy can be ~10^{52} erg and radio counterparts could be very bright.