Following the recommendation of the internal review, dithering is now used for all targets. ----- Attempting Submission 1 (Tue May 08 10:17:21 GMT 2007) ----- Phase II Proposal 11140 (vltp) successfully submitted. ----- Attempting Submission 2 (Mon May 21 10:35:23 GMT 2007) ----- This is a resubmission of proposal #68 due to the ACS failure Assigned ID: 1065 ----- Attempting Submission 1 (Tue Feb 06 09:19:10 GMT 2007) ----- Can mass-ejections from late He-shell flash stars constrain convective/reactive flow modeling of stellar interiors? 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.
We want to image faint nebular emission in the close vicinity of our five targets. The images shall be taken with WFPC2/PC1 and the F502N filter. We aim to fill the complete orbit. In order to avoid blooming, the exposures of targets 2 and 4 have to be split up into short exposures. The exposures of targets 1, 3, and 5 are split into two subexposures. This is sufficient for our purpose in order to correct for cosmic-particle contamination. Dithering is used for all targets. We used the WFPC2 ETC for point sources - v4.0 and determined the maximum exposure time to stay below the saturation level. For targets 2 and 4, the orbit planner is used then to get the maximum total exposure time. The target stars are the brightest objects in the FOV. N/A Standard calibration is sufficent for our purpose. 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