  Using the third-order WKB approximation, we evaluate the quasinormal
frequencies of massless scalar field perturbation around the black hole which
is surrounded by the static and spherically symmetric quintessence. Our result
shows that due to the presence of quintessence, the scalar field damps more
rapidly. Moreover, we also note that the quintessential state parameter
$\epsilon$ (the ratio of pressure $p_q$ to the energy density $\rho_q$) play an
important role for the quasinormal frequencies. As the state parameter
$\epsilon$ increases the real part increases and the absolute value of the
imaginary part decreases. This means that the scalar field decays more slowly
in the larger $\epsilon$ quintessence case.
