  This is the fourth paper of our series of works studying winds from hot
accretion flows around black holes. In the first two papers, we have shown the
existence of strong winds in hot accretion flows using hydrodynamical and
magnetohydrodynamical (MHD) simulations. In the third paper, by using three
dimensional general relativity MHD numerical simulation data of hot accretion
flows and adopting a "virtual particle trajectory" data analysis approach, we
have calculated the properties of wind, such as its mass flux and velocity.
However, that paper focuses only on a non-spinning black hole and SANE
(standard and normal accretion). In the present paper, we extend the third
paper by including cases of a rapidly rotating black hole and MAD (magnetically
arrested disk). We focus on investigating the effect of spin and magnetic field
on the properties of wind and jet. It is found that a larger spin and stronger
magnetic field usually enhance the wind and jet. The formulae describing the
mass flux, poloidal velocity, and fluxes of momentum, kinetic energy, and total
energy of wind and jet are presented. One interesting finding, among others, is
that even in the case of very rapidly spinning black hole where the jet is
supposed to be the strongest, the momentum flux of jet is smaller than that of
wind, while the total energy flux of jet is larger than that of wind by at most
a factor of 10. The implications of this result to the importance of wind
relative to jet in active galactic nuclei feedback are discussed.
