  We perform magnetohydrodynamic (MHD) simulations to investigate the
propagation of Alfven wave in magnetic chromosphere. We use the 1.5-dimensional
expanding flux tube geometry setting and transverse perturbation at the bottom
to generate the Alfven wave. Compared with previous studies, our expansion is
that we include the radiative loss term introduced by Carlsson & Leenaarts
(2012). We find that when an observation based transverse wave generator is
applied, the spatial distribution of the time-averaged radiative loss profile
in our simulation is consistent with that in the classic atmospheric model. In
addition, the energy flux in the corona is larger than the required value for
coronal heating in the quiet region. Our study shows that the Alfven wave
driven model has the potential to explain chromospheric heating and transport
enough energy to the corona simultaneously.
