POST Asymptotic Giant Branch Evolution in the Magellanic Clouds.

Details POST Asymptotic Giant Branch Evolution in the Magellanic Clouds. POST Asymptotic Giant Branch Evolution in the Magellanic Clouds.

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992hst..prop.3441d&link_type=abstract

HST Proposal ID #3441

Astronomy and Astrophysics

Astrophysics

Hst Proposal Id #3441

Scientific paper

Planetary Nebulae (PN) represent a critical stage of stellar evolution which is still poorly understood. We still lack reliable observational estimates of stellar luminosity, mass, effective temperature and age, which could be used to constrain evolutionary models, and determine key data such as mass-loss rates, He shell flash phases and the role of dredge-up. This proposal represents the first stage in a systematic and definitive study using HST observations, which will require approximately a further 150 hours for completion, of a large sample of nebulae at known distance in the Magellanic Clouds. The following observations allow us to derive all parameters needed for proper confrontation between theory and observation: * Direct PC imaging to detect central stars and to derive the physical dimensions, masses, ages, and spatial structure of the nebulae. * FOS spectrophotometry of the central stars and nebulae in the range 1150 - 2332 Angstroms. This data will be used in combination with stellar models to derive the effective temperature, bolometric luminosity, and mass of each of the exciting stars. The combination of these parameters with the dynamical age of the PN will define the evolutionary tracks in the Luminosity/T-eff diagram. We will use two independent ionisation codes to interpret the FOS spectra, optical and IR spectra, and the ionisation structure derived from the PC images. This analysis will yield chemical abundances of many elements, including the astrophysically important species He, C, N, O, and Si.

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