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Hot Gas in the Large Magellanic CloudThe Large Magellanic Cloud (LMC) offers an excellent laboratory to study the physical structure of the interstellar medium (ISM) because of its proximity, nearly face-on orientation, and small foreground and internal extinction. Optical and radio surveys of the LMC ISM have revealed interstellar structures of sizes ranging from a few parsecs to over 1000 parsecs. ROSAT X-ray mosaics of the LMC have detected abundant 10 (exp 6) K hot gas, some of which is bounded by large shell structures while the rest, does not appear to be associated with any visible interstellar structure. The X-ray observations have been analyzed to determine the physical conditions of the hot gas. The distribution of the hot gas can be compared to those of the cooler gas and massive stars, in order to determine the production mechanism of the hot gas. UV observations of interstellar absorption lines of high ions, such as C IV, N V, and O VI, can be used to study the interfaces between the 10 (exp 6) K gas and cooler ionized gas, and to provide constraints on the location of 10 (exp 6) K gas with respect to the cooler gas along the line of sight.
Document ID
20000090654
Acquisition Source
Goddard Space Flight Center
Document Type
Conference Paper
Authors
Chu, You-Hua
(Illinois Univ. Urbana-Champaign, IL United States)
Date Acquired
August 19, 2013
Publication Date
May 1, 2000
Publication Information
Publication: Astrophysical Plasmas: Codes, Models, and Observations
Volume: 9
Subject Category
Astrophysics
Funding Number(s)
CONTRACT_GRANT: NAG5-3246
CONTRACT_GRANT: NAG5-7003
CONTRACT_GRANT: GO-06698.01-95A
Distribution Limits
Public
Copyright
Other

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