  The time-scales of the variabilities in changing look (CL) active galactic
nuclei (AGNs) are usually at the order of years to tens of years (some of them
are even shorter than one year), which are much shorter than the viscous
timescale of a standard thin accretion disk. It implies that the variabilities
of CL AGNs cannot be reproduced by varying the mass accretion rate of the thin
disk. In this work, we employ a magnetic accretion disk-outflow model to
calculate the inflow time of the disk predominantly driven by magnetic
outflows. In this model, most angular momentum of the gas in the disk is
carried away by the outflows, and therefore its radial velocity can be
substantially higher than that of a conventional viscous disk. Our calculations
show that the inflow time of such a disk with outflows can be around several
years to tens years. The calculated spectra of the disk with outflows can fit
the observed spectra of a CL AGN Mrk 1018 quite well both in the low and high
states. The derived inflow time of such a disk with outflows is around 5 years
in the high state, while it becomes $\sim 20$ years in the low state, which is
roughly consistent with the observations of the variabilities in Mrk 1018.
