Stellar Activity in 1231 Northern Hemisphere Stars
purpose: Use chromospheric activity markers to determine rotation periods and ages for many FGK and M type stars
This paper describes the mathematical method behind using Ca II H &K lines to predict stellar rotational period.
In the paper, I saw that this method is only calibrated for stars with B-V between 0.44 and 0.9. This means that it won't be useful for M stars. I investigated Noyes et al. 1984 to figure out why, and found that continuum bandpasses for stars with B-V>0.9 were "heavily line blanketed" and therefore the S-value could not be calculated. It is possible that if the entire process could be calibrated for V-I or some color indicator different from B-V, chromospheric activity could be used to calculate P, and therefore age.
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