  We construct an analytical black hole accretion disk model that incorporates
both magnetic pressure and disk wind, which are found to be important from
numerical simulations. A saturated magnetic pressure that relates the Alfven
velocity with local Keplerian velocity and gas sound speed is assumed in
addition to radiation and gas pressures. The mass accretion rate is assumed to
have a power-law form in response to mass loss in the wind. We find three sets
of self-consistent solutions that are thermally stable and satisfy the model
assumptions. At high accretion rates, the disk is geometrically and optically
thick, resembling the slim disk solution. At relatively low accretion rates,
our model predicts an accretion flow consisting of a geometrically thin and
optically thick outer disk (similar to the standard disk), and a geometrically
thick and optically thin inner disk (similar to the advection-dominated
accretion flow or ADAF). Thus, this is a natural solution for a truncated disk
connected with an inner ADAF, which has been proposed to explain some
observations. The magnetic pressure plays a more important role than the
outflow in shaping the disk structure. The observed disk luminosity tends to
saturate around 8 times the Eddington limit, suggesting that supercritical
accretion onto black holes can be used for black hole mass estimate, or a
standard candle with known black hole masses.
