Computer Science – Sound
Scientific paper
May 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000rmxac...9....1s&link_type=abstract
Astrophysical Plasmas: Codes, Models, and Observations, Proceedings of the conference held in Mexico City, October 25-29, 1999,
Computer Science
Sound
Scientific paper
Major advances have been made in the past decade in our knowledge of the hot interstellar gas of our Milky Way galaxy. The Diffuse X-ray Spectrometer obtained spectra in the 0.15-0.28 keV range from the Galactic plane (i.e., from the Local Bubble) that show emission lines and blends. These spectra confirm that the soft X-ray background in this energy range is thermal in origin, at temperature roughly 106 K, but the spectra are not well fit by standard plasma emission models. Data from the ROSAT satellite, both from the all-sky survey and from pointed observations, have provided constraints on the distances to some of the hot gas emitting regions in the Local Bubble, the local ISM, and the Galactic halo. These data confirm that the local bubble is ~100 pc in size, and they indicate the existence of two independent hot gas components in the Galactic halo: a patchy, localized lower temperature halo component near 106 K, and a smoother higher temperature halo component at several 106 K, with a spatial structure reflective of the overall structure of the galaxy. The asca\ satellite has observed emission from hot plasmas at temperatures above 107 K from the Galactic ridge, from two different galactic center components, and from the Galactic bulge. More recently, the Wisconsin/Goddard micro-calorimeter sounding rocket payload has observed the spectrum of the diffuse emission from (l,b)~(90o,60o) with a 1 sr field of view over the 0.1-1 keV spectral range with ~ 8 eV resolution. Lines from O VII and O VIII are clearly seen, but there are only upper limits to the expected Fe XVII lines.
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