Hi guys, I am dealing with the following issue: in low mass stars during the main sequence, the core gets filled with He ashes over time until the pressure is not sufficient to keep it in hydrostatic balance. Then the core starts to contract on KH timescale until it hits the full degeneracy where the contraction stops and the star becomes a WD. My question is: what is the density of the He core just before it reaches the Schonberg-Chandrasekhar limit? Is it the same as the initial H core density of ~200g/cm3? Or does it change as more He is added over time? Thank you.