Excitation Mechanisms and Abundances in the O-Rich SNR E0102.2--7219 in the SMC

Details Excitation Mechanisms and Abundances in the O-Rich SNR E0102.2--7219 in the SMC Excitation Mechanisms and Abundances in the O-Rich SNR E0102.2--7219 in the SMC

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.6052m&link_type=abstract

HST Proposal ID #6052

Computer Science

Hst Proposal Id #6052 Interstellar Medium

Scientific paper

We propose to obtain WFPC2 images and FOS spectra of theyoung, oxygen-rich supernova remnant E0102.2--7219 in theSmall Magellanic Cloud. The images will be used to study thefine-scale spatial and ionization structures within the knottyfilaments, and also provide EARLY ACQ exposures for thespectroscopy. The FOS spectra will provide relativeintensities of UV and optical emission lines in isolatedknots. Only HST has the resolving power necessary to studyindividual knots in the remnant. We will compare the observedline ratios to predictions made by theoretical models in orderto determine the excitation mechanisms and to derive reliableelemental abundances. E0102.2--7219 is one of only two O-richsupernova remnants that can be studied effectively at UVwavelengths, and the HST data will provide important tests fortheories of nucleosynthesis in massive stars as well asimprove our understanding of the dynamics of supernovaexplosions and mixing in the ejecta. We will compare thesedata to our HST Cycle 4 observations of N132D in the LMC toinvestigate differences between these SNRs apparent in the IUEspectra.

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