Gyrochronology is a method of deriving the age of a cool main sequence star
from its measured rotation period, itself derived from photometric time-series
observations from the ground or from space.
Although derived originally using observations of open cluster stars, it can
potentially be applied on a massive scale to field stars, including exoplanet
hosts.
I will relate the empirical origins of gyrochronology, and connect these to
relevant theoretical issues in cool star rotation and activity.
A hybrid of theoretical and observational approaches seems to promise the best
ages, including pointers for suppressing errors in age determination methods,
and insights into the underlying stellar physics.
Finally, I will outline how small surveys are changing, and large surveys could
potentially revolutionize, our understanding of stellar ages.
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