PG1159 stars are hot pre-white dwarfs characterized by a surface composition that consists almost entirely of He, C and O. Most of them are the result of the occurrence of late helium shell flashes after departure from the AGB. Below, we provide links to a complete set of evolutionary and pulsational computations of PG1159 pre-white dwarf models calculated from the ZAMS. Our calculations cover a wide mass range.

Evolutionary tracks of PG1159 stars