  The ubiquitous interstellar turbulence regulates star formation and the
scaling relations between the initial velocity differences and the initial
separations of stars. We propose that the formation of wide binaries with
initial separations $r$ in the range $\sim 10^3~\text{AU} \lesssim r \lesssim
10^5$ AU is a natural consequence of star formation in the turbulent
interstellar medium. With the decrease of $r$, the mean turbulent relative
velocity $v_\text{tur}$ between a pair of stars decreases, while the largest
velocity $v_\text{bon}$ at which they still may be gravitationally bound
increases. When $v_\text{tur} < v_\text{bon}$, a wide binary can form. In this
formation scenario, we derive the eccentricity distribution $p(e)$ of wide
binaries for an arbitrary relative velocity distribution. By adopting a
turbulent velocity distribution, we find that wide binaries at a given initial
separation generally exhibit a superthermal $p(e)$. This provides a natural
explanation for the observed superthermal $p(e)$ of the wide binaries in the
Solar neighborhood.
