Physical Conditions of Interstellar Gas Within 50 Parsecs

Details Physical Conditions of Interstellar Gas Within 50 Parsecs Physical Conditions of Interstellar Gas Within 50 Parsecs

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991hst..prop.2537f&link_type=abstract

HST Proposal ID #2537

Physics

Hst Proposal Id #2537

Scientific paper

Models of the diffuse interstellar medium still lack definite observational proofs, in particular on small scale lengths (<10pc). They predict interfaces between cold dense clouds and a hot "coronal" very tenuous widely spread phase. These interfaces need to be directly obseved and studied because they offer a unique chance to understand the role of shocks, the nature of the evaporation zones, the grain destruction, the extent of the warm gas phase. All these problems can only tackled in details in the very local interstellar medium where the low column-densities of individual absorption regions are not hidden and can be well enough located. From ground-based studies, we have pointed out a new image of the nearby instellar medium. At least four velocity components are present within 20 pc. For two of them, we were able to delineate approximate frontiers toward which it is very promissing to search for interfaces. Furthermore, we found some evidence for a temperature structure within one of these components, providing therefore a prime target. Since visual observations do not offer adequate diagnostic lines and available UV data do not have the needed spectral resolution, we propose to perform with HRS a much more complete physical study of the cold and warm local gas. The selected diagnostic lines are those of AlII, FeII, MnII, MgI, and CIV, to be observed toward nearby stars in directions where confusion betwee

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