Morphology of High Radio Surface Brightness Planetary Nebulae

Details Morphology of High Radio Surface Brightness Planetary Nebulae Morphology of High Radio Surface Brightness Planetary Nebulae

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8307k&link_type=abstract

HST Proposal ID #8307

Mathematics

Logic

Hst Proposal Id #8307 Stellar Ejecta

Scientific paper

The morphological transformation from the spherically symmetric circumstellar envelopes of AGB stars to the complex, bipolar structures of planetary nebulae has remained one of the major unresolved problems in the late stages of stellar evolution. Recent HST observations of proto-planetary nebulae and planetary nebulae have found evidence for jets and radial filaments suggesting that non-isotropic outflows are occuring during the early stages of planetary nebula evolution. However, the morphology of very young planetary nebulae have not been extensively studied by the HST. In this proposal, we have selected a group of compact {< 2^ } and high radio surface brightness planetary nebulae to image in three narrow bands {HAlpha, N ii, and O iii} to determi ne the morphological structures as a function of ionization. With these images, we should be able to detect any previously unseen haloes, arcs, jets, and knots, and derive the physical conditions of these features at the ea rliest stage of PN evolution.

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