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Tidal friction has long been recognized to circularize the orbits of binarystars over time. In this study, we use the observed distribution of orbitaleccentricities in populations of binary stars to probe tidal dissipation. Incontrast to previous studies, we incorporate a host of physical effects oftenneglected in other analyses, provide a much more general description of tides,model individual systems in detail (in lieu of population statistics), andaccount for all observational uncertainties. The goal is to provide a reliablemeasurement of the properties of tidal dissipation that is fully supported bythe data, properly accounts for different dissipation affecting each tidal waveon each object separately, and evolves with the internal structure of thestars. We extract high precision measurements of tidal dissipation in shortperiod binaries of Sun-like stars in three open clusters. We find that thetidal quality factor on the main sequence falls in the range $5.7 <\log_{10}Q_\star' < 6$ for tidal periods between 3 and 7.5 days. In contrast,the observed circularization in the 150 Myr old M 35 cluster requires thatpre-main sequence stars are much more dissipative: $Q_\star' < 4\times10^4$. Wetest for frequency dependence of the tidal dissipation, finding that for tidalperiods between 3 and 7.5 days, if a dependence exists, it is sub-linear formain-sequence stars. Furthermore, by using a more complete physical model forthe evolution, and by accounting for the particular properties of each system,we alleviate previously observed tensions in the circularization in the openclusters analyzed.

Comprehensive Bayesian Modeling of Tidal Circularization in Open Cluster Binaries part I: M 35, NGC 6819, NGC 188