Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...434..599s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 434, no. 2, p. 599-613
Astronomy and Astrophysics
Astronomy
59
Absorption Spectra, Astronomical Models, Bubbles, Interstellar Gas, Mass Distribution, Oxygen Ions, Space Density, Ultraviolet Astronomy, Ultraviolet Spectra, Computerized Simulation, Oao 3, Statistical Analysis, Stellar Winds, Supernova Remnants
Scientific paper
The Copernicus O(+5) column densities toward 72 stars provide a rare and valuable tracer of 105.5 K gas in the interstellar medium. The original analysis of the data by Jenkins provided important clues about the distribution of interstellar O(+5) ions, but our understanding of the local interstellar medium has since grown substantially. We revisit that work, including the possibility that local hot gas may contribute a significant O(+5) column density to most lines of sight. Our reanalysis also includes slight improvements in the statistics and was found to be reliable when tested on simulated data sets. In the end, we come to conclusions about the distribution of interstellar O(+5) ions that differ considerably from those of the original analysis. With our reanalysis, some theoretical models now show promise. For example, our Local Bubble column density compares favorably with the estimated quantity of O(+5) within the remnant of an ancient local explosion. Similarly, our mean O(+5) column density per feature in more distant regions is like that found in models of hot interstellar bubbles from either stellar winds or ancient supernova explosions in a warm diffuse interstellar environment, suggesting that the hot gas in interstellar space may exist primarily within discrete regions of modest volume occupation rather than in a continuous and pervasive phase.
Cox Donald P.
Shelton Robin L.
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