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. 2015 Feb 1;15(2):119–143. doi: 10.1089/ast.2014.1231

FIG. 3.

FIG. 3.

Evolution of the position of the inner edge of the empirical HZ (RV limit) as a function of time. Left: Location of the RV limit versus stellar age for stars between 0.08 M⊙ and 1 M⊙. The vertical dashed line corresponds to the 10 Myr formation time assumed in our model. Right: Contours of the RV limit on a classical HZ plot between 3 Myr (black line) and 1 Gyr (orange line). The empirical HZ at 1 Gyr is shaded in blue for reference. Note that the inner edge moves in by about an order of magnitude for the lowest-mass M dwarfs.