Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8344b&link_type=abstract
HST Proposal ID #8344
Astronomy and Astrophysics
Astrophysics
Hst Proposal Id #8344 Field Stellar Populations
Scientific paper
Metallicity is the most fundamental parameter governing both stellar and galactic evolution. Yet, little is known observationally about how metallicity affects the physics of massive stars. To explore this connection, we will use the STIS to obtain slitless UV spectroscopy of bright OB associations in three Local Group galaxies that span a factor of 30 in metallicity. Our targets are star-forming regions in M31, NGC 6822, and Sextans A. Nebular O/H abundances indicate Sextans A is the most metal deficient galaxy in the Local Group, with a metallicity 30x below the Galaxy and 3x below the SMC. The STIS UV slitless spectra will resolve numerous O and B stars in a single exposure. This study will use the unique spectral imaging capabilities of STIS to probe stellar populations spanning the widest range of metallicity possible. Theoretical synthetic spectra will be constructed in an attempt to match the strengths and shapes of both strong photospheric and wind features. In th is way we will derive approximate abundances, mass loss rates, and terminal velocities. We will also apply our new UV stellar classification criteria and probe the variation with metallicity of mass-loss characteristics through the H-R diagram. Our goal is to answer one of the most fundamental questions in astrophysics: ``What is the impact of chemical abundance upon stellar mass loss?"
No associations
LandOfFree
UV Spectral Properties of O and B Stars Versus Metallicity does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with UV Spectral Properties of O and B Stars Versus Metallicity, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and UV Spectral Properties of O and B Stars Versus Metallicity will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-993298