The Early Onset of Asymmetric Outflow During the Planetary Nebula Formation Process

Details The Early Onset of Asymmetric Outflow During the Planetary Nebula Formation Process The Early Onset of Asymmetric Outflow During the Planetary Nebula Formation Process

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6366t&link_type=abstract

HST Proposal ID #6366

Computer Science

Hst Proposal Id #6366 Interstellar Medium

Scientific paper

We propose to study early mass loss in the planetary nebula {PN} formation process using the high resolution imaging capabilities of HST. While tremendous progress has been made in understanding the late stages of PN formation, the details of the earliest phases of this metamorphosis are still vague. A knowledge of the characteristics of the mass loss occurring as a star leaves the asymptotic giant branch {AGB} is crucial to a complete picture of the PN development, since early mass loss is thought to determine the final shape of an object by confining the faster winds that occur later in the formation process. Unfortunately, there is little observational evidence that probes the distribution of this early ejecta. Is the final morphology of a PN imprinted at early times as suggested by the formation models? Fully developed PNe display a variety of morphologies ranging from round to bipolar. Based on the formation models we might expect material ejected early in the development of a PN to also exhibit a range of morphologies. Is this what we observe? We will directly address these questions by obtaining PC2 images of a sample of AGB/post-AGB stars. We have shown, using polarimetry, that the stars in this sample possess extended scattering envelopes that are spatially unresolved from the ground, but can be resolved using HST. These observations will reveal the morphology of the ejecta in the first stages of the PN formation process, thus testing the validity of the current models of PN formation.

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