What is the origin of H-deficient post-AGB stars?

Details What is the origin of H-deficient post-AGB stars? What is the origin of H-deficient post-AGB stars?

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005cxo..prop.1891w&link_type=abstract

Chandra Proposal ID #07200459

Physics

Chandra Proposal Id #07200459

Scientific paper

PG1159 stars are extremely hot, hydrogen-deficient (pre-) white dwarfs. The origin of their exotic surface abundance pattern is still debated. The C, He, O dominated atmospheres suggest that they suffered a late helium-shell flash, which causes ingestion and burning of the hydrogen-rich surface layer and the dredge-up of 3-alpha processed matter. Some PG1159 stars are non-radial pulsators and their pulsation properties reveal their interior structure. This gives the unique possibility to uncover their true evolutionary history. A prerequisite of pulsation studies is the knowledge of their position in the HRD. A Chandra observation of the non-pulsator PG1520+525 allows a very accurate T-eff determination, enabling us to confine the blue edge of the instability strip.

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