How did Stars Evolve in the Early Universe? , the Role of Metallicity

Details How did Stars Evolve in the Early Universe? , the Role of Metallicity How did Stars Evolve in the Early Universe? , the Role of Metallicity

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6687h&link_type=abstract

HST Proposal ID #6687

Computer Science

Hst Proposal Id #6687 Hot Stars

Scientific paper

Using GHRS spectra of post-AGB stars, we propose to test andrefine a new evolutionary scheme for low- and intermediate-mass stars. This scheme takes into account the effect ofmetallicity on mass-loss in all evolutionary phases, includingdust-enhanced mass loss on the asymptotic giant branch (Bowen1988), pulsation-enhanced mixing and mass-loss (Gautschy1993), and radiation-driven winds in the post-AGB phase (Heap1986). In the transition between the AGB and CSPN phases, astar with a high metallicity (i.e. solar abundance) may bestripped of its H-rich envelope and thereby become a He-Cenriched star with a Wolf-Rayet spectral type; whereas a low-Zand/or low-mass post-AGB star should pass through this stageunscathed and thus appear as a normal O or Of-type star. Totest this scenario, we will determine the rate of mass-lossand iron abundance of O and WR-type post-AGB stars bycomparing detailed NLTE models of the photosphere and wind tohigh S/N spectra obtained by GHRS. We will then construct newevolutionary tracks that take proper account of mass-loss andmixing. These results will be applied to disparateenvironments, such as the low-metal environment of theMagellanic Clouds and the high-metal environment of ellipticalgalaxies with ultraviolet excesses.

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