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The heavy mass loss observed in evolved asymptotic giant branch (AGB) starsis usually attributed to a two-stage process: atmospheric levitation bypulsation-induced shock waves, followed by radiative acceleration of newlyformed dust grains. The dust transfers momentum to the surrounding gas throughcollisions and thereby triggers a general outflow. Radiation-hydrodynamicalmodels of M-type AGB stars suggest that these winds can be driven by photonscattering -- in contrast to absorption -- on Fe-free silicate grains of sizes0.1--1\,$\mu$m. In this paper we study photometric constraints for wind-drivingdust species in M-type AGB stars, as part of an ongoing effort to identifylikely candidates among the grain materials observed in circumstellarenvelopes. To investigate the scenario of stellar winds driven by photonscattering on dust, and to explore how different optical and chemicalproperties of wind-driving dust species affect photometry we focus on two setsof dynamical models atmospheres: (i) models using a detailed description forthe growth of Mg$_2$SiO$_4$ grains, taking into account both scattering andabsorption cross-sections when calculating the radiative acceleration, and (ii)models using a parameterized dust description, constructed to representdifferent chemical and optical dust properties. By comparing syntheticphotometry from these two sets of models to observations of M-type AGB stars wecan provide constraints on the properties of wind-driving dust species.Photometry from wind models with a detailed description for the growth ofMg$_2$SiO$_4$ grains reproduces well both the values and the time-dependentbehavior of observations of M-type AGB stars, providing further support for thescenario of winds driven by photon scattering on dust.

Exploring wind-driving dust species in cool luminous giants II. Constraints from photometry of M-type AGB stars