Evolutionary sequence for a hydrogen deficient post-born again star of 0.5885 Msun as described in Althaus, Serenelli, Panei et al. 2005, A&A, 435, 631, is provided. Calculations have been done with the stellar evolutionary code LPCODE developed at University of La Plata, Argentina and described in the above mentioned paper. The sequence is computed selfconsistently from an initially 2.7 Msun progenitor star evolved from the ZAMS through the core hydrogen- and helium-burning evolutionary phases to the thermally pulsing AGB and, ultimately, to the born again episode that is responsible for the hydrogen deficiency. White dwarf sequences are computed in a consistent way with the evolution of chemical abundance distribution caused by element diffusion along the whole cooling phase. Calculations are extended down to an effective temperature of 7000 K. The full treatment of the entire evolutionary history of white dwarfs provides a consistent white dwarf initial configuration. Note: Updated evolutionary sequences of hydrogen-deficient white dwarfs for different stellar masses can be found at Althaus et al. 2009

The cooling sequence file lists from left to right:

The logarithm of the surface luminosity in solar unit;

The logarithm of the effective temperature (K);

The logarithm of age counted from the moment at which the remnant reaches Teff=10,000K (after the occurrence of the double loop at high luminosity);

The logarithm of stellar radius (cm)

The logarithm of the surface gravity

The logarithm of helium-burning luminosity in solar unit

The HR diagram for the whole evolutionary stages from the ZAMS to the WD is shown in the figure below.