In this work, we investigate the near $2:1$ mean motion resonance capture scenario and tidal evolution for the hot-Neptune system HD 106315 by numerical simulations. To make a deeper understanding of migration for this system, we extensively explore the initial semi-major axis, eccentricity, as well as the attenuation coefficient of the eccentricity of HD 106315c affecting the orbital configuration of the system. The numerical simulations show that when the initial orbital elements of two planets are $a_b\sim0.4$au, $a_c\sim0.8$au, $e_b$ and $e_c$ lower than 0.03, HD 106315b and HD 106315c can migrate to currently observed location, and form near $2:1$ mean motion resonance. This scenario takes into account the effect of the central star and the viscosity of disk.\qquad In addition, tidal dissipation that originates from the host star, can influence the mean motion resonant configuration for planets. From a viewpoint of theoretical analysis and simulations, the results show that for tidal dissipation factor $Q = 100 $, the ratio of orbital period of two planets will change over the evolution. This may be indicative of the resonant departure for two planets in the system. However, tidal dissipation factor Q may be larger than $10^3$ for the planets, therefore we may safely conclude that tidal effect does not play a major role in driving two Neptunian planets of the HD 106315 system move out of $2:1$ mean motion resonance within the residual lifetime of the star.