Abstract
A brief summary of previous work emphazises the evidence for an origin of the Magellanic Stream (MS) by ram-pressure sweeping of gas from the Magellanic Clouds (MCs) and the Inter Cloud Region (ICR) by coronal galactic gas. Further we present results of recent investigations of the physical conditions of the diffuse gas and dust in the halo of the MCs and the MS. HI emission and absorption studies, carried out with the Parkes 64-m telescope and the Australia Telescope (AT) indicate that the spin temperature of the HI gas in the halo of the MCs and in the MS is warmer than that in the outer parts of our Galaxy. An unsuccessful search for IRAS 100 μm micron emission in the H I halo of the SMC and in a number of fields in the MS indicates a rater low intensity of the ambient radiation field. Detection of IR emission in an IVC and an HVC associated with the MS supports ram pressure models for the origin of the MS.
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Ulrich, M., Uwe, H. (1992). Recent Studies of Gas and Dust in the Magellanic System. In: Baschek, B., Klare, G., Lequeux, J. (eds) New Aspects of Magellanic Cloud Research. Lecture Notes in Physics, vol 416. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-56432-2_175
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DOI: https://doi.org/10.1007/3-540-56432-2_175
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