POST Asymptotic Giant Branch Evolution in the Magellanic Clouds - Spectroscopy: Cycle 4 High

Details POST Asymptotic Giant Branch Evolution in the Magellanic Clouds - Spectroscopy: Cycle 4 High POST Asymptotic Giant Branch Evolution in the Magellanic Clouds - Spectroscopy: Cycle 4 High

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994hst..prop.5736d&link_type=abstract

HST Proposal ID #5736

Astronomy and Astrophysics

Astrophysics

Hst Proposal Id #5736 Interstellar Medium Planetary Nebulae

Scientific paper

Planetary Nebulae (PN) represent a critical stage of stellar evolution which is relatively poorly understood. More reliable observational estimates of stellar luminosity, mass, effective temperature, and age are required to constrain evolutionary models and determine mass-loss rates, He shell flash phases, and the role of dredge-up. This proposal represents the continuation of our systematic and definitive study with HST of a large sample of nebulae at known distance in the Magellanic Clouds and requires approximately 50 hours for completion. All parameters needed for confrontation of theory with observation can be derived from direct PC imaging and FOS spectra in the 1150-3200A range. The images give spatial structure, sizes, ionized mass, dynamical ages, and an estimate of the final mass-loss rate on the AGB. The spectra will be combined with the images and with stellar atmospheric and evolutionary models to derive the effective temperature, luminosity, and core mass of each of the exciting stars. These data will define the evolutionary status of each of the PN observed. We will use two independent ionization codes to interpret the spatial structure derived from PC images and the FOS data, in conjuction with optical and IR spectra. This analysis will also yield chemical abundances of many elements, including the astrophysically important species He, C, N, O, and Si.

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