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We utilize Kepler data to study the precision differential photometricvariability of solar-type and cooler stars at different timescales, rangingfrom half an hour to 3 months. We define a diagnostic that characterizes themedian differential intensity change between data bins of a given timescale. Weapply the same diagnostics to SOHO data that has been rendered comparable toKepler. The Sun exhibits similar photometric variability on all timescales ascomparable solar-type stars in the Kepler field (it is not unusually quiet).The previously-defined photometric "range" serves as our activity proxy (drivenby starspot coverage). We revisit the fraction of comparable stars in theKepler field that are more active than the Sun. The exact active fractiondepends on what is meant by "more active than the Sun", and on the magnitudelimit of the sample of stars considered. This active fraction is between aquarter and a third (depending on the timescale). We argue that a reliableresult requires timescales of half a day or longer and stars brighter thanKepler magnitude of 14, otherwise non-stellar noise distorts it. We alsoanalyze main sequence stars grouped by temperature from 6500-3500K. As onemoves to cooler stars, the active fraction of stars becomes steadily larger(greater than 90% for early M dwarfs). The Sun is a good photometric model atall timescales for those cooler stars that have long-term variability withinthe span of solar variability.

Photometric Variability in Kepler Target Stars. III. Comparison with the Sun on Different Timescales