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We present an analysis of debris disk data around Solar-type stars (spectraltypes F0-K5) using the steady-state analytical model of Wyatt et al. (2007).Models are fitted to published data from the FEPS (Meyer et al. 2006) projectand various GTO programs obtained with MIPS on the Spitzer Space Telescope at24 micron and 70 micron, and compared to a previously published analysis ofdebris disks around A stars using the same evolutionary model. We find that themodel reproduces most features found in the data sets, noting that the modeldisk parameters for solar-type stars are different to those of A stars.Although this could mean that disks around Solar-type stars have differentproperties from their counterparts around earlier-type stars, it is alsopossible that the properties of disks around stars of different spectral typesappear more different than they are because the blackbody disk radiusunderestimates the true disk radius by a factor $X_r$ which varies withspectral type. We use results from realistic grain modelling to quantify thiseffect for solar-type stars and for A stars. Our results imply thatplanetesimals around solar-type stars are on average larger than around A starsby a factor of a few but that the mass of the disks are lower for disks aroundFGK stars, as expected. We also suggest that discrepancies between theevolutionary timescales of 24 micron statistics predicted by our model and thatobserved in previous surveys could be explained by the presence oftwo-component disks in the samples of those surveys, or by transient eventsbeing responsible for the 24 micron emission of cold disks beyond a few Myr.Further study of the prevalence of two component disks, and of constraints on$X_r$, and increasing the size of the sample of detected disks, are importantfor making progress on interpreting the evolution of disks around solar-typestars.

Steady-state evolution of debris disks around solar-type stars