Can mass-ejections from late He-shell flash stars constrain convective/reactive flow modeling of stellar interiors?

Details Can mass-ejections from late He-shell flash stars constrain convective/reactive flow modeling of stellar interiors? Can mass-ejections from late He-shell flash stars constrain convective/reactive flow modeling of stellar interiors?

Jul 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007hst..prop11140w&link_type=abstract

HST Proposal ID #11140. Cycle 16

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Scientific paper

The existence of H-deficient knots around the central stars of the planetary nebulae Abell 30 and Abell 78 is still unexplained. We hypothesize that these knots were ejected during a very late helium-shell flash = very late thermal pulse, VLTP suffered by the precursor white dwarf stars. If this is true, then the characteristics of these knots mass, velocity, density, spatial distribution allow to draw conclusions on the course of the hydrogen-ingestion flash detonation that is triggered by the He-shell flash. This provides important, otherwise inaccessible constraints for the hydrodynamical modeling of convective/reactive flows in stellar interiors. Understanding the physics of these flows is not only important for the understanding of these particular central stars, but also for the frequent, very similar convective/reactive events that determine the nucleosynthesis in Pop. III stars. With this proposal we want to proof or discard the idea that the H-deficient knots are resulting from a VLTP. If true, then they can be exploited for flash-physics diagnostics. We propose a simple test. We search for such knots around five H-deficient central stars PG1159 stars. Our models predict, that only those stars with residual nitrogen in the atmosphere have suffered a VLTP and, hence, should have expelled knots. We therefore want to take [O III] images of stars which have photospheric N and those which do not.;

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