Uv Spectroscopy of DR 1, the WO3 Star in IC 1613 and its Surrounding Nebula, S3

Details Uv Spectroscopy of DR 1, the WO3 Star in IC 1613 and its Surrounding Nebula, S3 Uv Spectroscopy of DR 1, the WO3 Star in IC 1613 and its Surrounding Nebula, S3

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6622k&link_type=abstract

HST Proposal ID #6622

Physics

Hst Proposal Id #6622 Hot Stars

Scientific paper

We propose to obtain UV FOS and GHRS spectra ofDR 1, a very luminous WO type Wolf-Rayet star in the metal-poor dwarf irregular galaxy IC 1613. Simultaneously, we willobtain spectra of a portion of S3, its surrounding nebula.The stellar spectra will be analysed using a sophisticated non-LTE radiative transfer code, allowing for sphericalextension, stellar winds and non-LTE line blanketing, todetermine C/He and O/C abundance ratios which will provideconstraints on the He-burning stage of evolution of massivestars. Our quantitative analysis will also yield fundamentalphysical parameters such as terminal velocity, mass-loss rateand luminosity, thereby allowing tight constraints to beplaced on massive star evolutionary theory at very lowmetallicities. At Z=0.001, IC 1613 is the lowest metallicityregion known to house such an evolved massive star. Acomplementary nebular analysis will yield abundances of N^2+,N^3+, N^4+, C^+, C^2+, C^3+, and O^3+ relative to H^+ (ionswhich are only observable in the UV), enabling an accuratetotal abundance analysis in conjunction with existing opticalspectra. The UV nebular carbon lines provide the only means ofderiving the nebular carbon abundance for this low metallicityregion. In addition, a Zanstra and Stoy temperature analysiswill be used to constrain the stellar temperature adopted forthe non-LTE model, enabling a more accurate overall analysis.HST provides the only means of obtaining UV spectra of DR 1and S3.

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