This directory contains files with thermodynamic and chemical structures of SNIa progenitor models. i.e.
accreting white dwarfs whose masses have approached the Chandrasekhar limit.
The initial masses of the stars are 6.3 and 6.9 Msun. The first WD is a pure CO one, while the second is a hybrid one.
The files with the word "chem" at the end of their names provide the mass coordinate in Msun followed by
mass fractions of 12C, 16O, 20Ne, 22Ne, 23Na, 24Mg and 25Mg. The other files give the radius in cm,
density in g/cm^3, temperature in K, mass coordinate in Msun and the exact value of Y_e from the MESA
models.

The files with no special comments in their names correspond to our standard computations that included
both convective boundary mixing and Urca processes.

The files with the word "limited" in their names are obtained assuming that the Urca process limits the mass of
the convective core, as described in our paper at arXiv:1407.0248 [astro-ph.SR] (see Fig. 8).