Watching Young Planetary Nebulae Grow: The Movie
The development of magneto-hydro gas dynamical models is the key to the understanding of both the physics (processes) and astronomy (initial conditions) of astrophysical nebulae of all sorts. The models are reaching their highest degree of accuracy when applied to and compared against pre Planetary Nebulae (pPNe) thanks to the simplicity, relative lack of extinction, and the detail of the imaging and kinematic data that have bcome available for these objects.
The primary barrier to progress is inadequate kinematic data of pPNe against which the predictions models can be tested. Unlike PNe, pPNe do not emit emission lines for detailed Doppler measurements. Therefore it is essential to find another way to monitor the morphological evolution.
Only HST can uncover the dynamics of the growth patterns by subtracting multi-epoch images spanning a decade or more. We have selected four pPNe with highly collimated outflows in different evolutionary stages for which high-quality first-epoch images were obtained from 1996 to 2002. All of them display regularly shaped thin rims, sharp edges, and symmetric pairs of knots or bowshocks that are ideal for our purposes. We will closely mimic many of the earlier exposures using ACS and to monitor changes in structures. The morphology and its evolution will be compared to 3-D MHD models with adaptive grids in order to build a far clearer picture of the nuclear geometry which shaped the outflows and constrained their propagation to the present. We shall also obtain R, J, and H images for use with a 3-D dust radiative transfer code LELUYA to model the dust distribution deep into the nuclear zones.
The program emulates imaging observations of the targets taken about 10 years earlier. Differences in the old and new images reveal the growth patterns which, in turn, illuminate the process that are shaping the outflows from these post-AGB stars.
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