  We perform neutrino radiation-hydrodynamics simulations for the merger of
asymmetric binary neutron stars in numerical relativity. Neutron stars are
modeled by soft and moderately stiff finite-temperature equations of state
(EOS). We find that the properties of the dynamical ejecta such as the total
mass, neutron richness profile, and specific entropy profile depend on the mass
ratio of the binary systems for a given EOS in a unique manner. For the soft
EOS (SFHo), the total ejecta mass depends weakly on the mass ratio, but the
average of electron number per baryon ($Y_e$) and specific entropy ($s$) of the
ejecta decreases significantly with the increase of the degree of mass
asymmetry. For the stiff EOS (DD2), with the increase of the mass asymmetry
degree, the total ejecta mass significantly increases while the average of
$Y_e$ and $s$ moderately decreases. We find again that only for the soft EOS
(SFHo), the total ejecta mass exceeds $0.01M_\odot$ irrespective of the mass
ratio chosen in this paper. The ejecta have a variety of electron number per
baryon with its average approximately between $Y_e \sim 0.2$ and $\sim 0.3$
irrespective of the EOS employed, which is well-suited for the production of
the r-process heavy elements (second and third peaks), although its averaged
value decreases with the increase of the degree of mass asymmetry.

High Energy Astrophysical Phenomena;Cosmology and Nongalactic Astrophysics;Solar and Stellar Astrophysics;General Relativity and Quantum Cosmology