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Fig. C.1.

image

Hertzsprung-Russell diagram showing the evolution of five stars that become stripped through mass transfer with a companion star. We show the evolution for models of donor stars with initial masses of 2.7, 5.45, 8.15, 12.17, and 18.17 M, labeled as such. The tracks are gray for all but the central helium burning phase (defined as when the central helium mass fraction is between 0.9 and 0.1), which is colored with the central mass fraction of helium. The colored regions cover only a small part of the HR diagram and therefore indicates that the stripped stars have similar stellar parameters throughout the stripped phase. The models have solar metallicity. (We show here the surface temperature T, which is referred to as the effective temperature in MESA).

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