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J. E. Vaillancourt (U. Wisconsin - Madison)
The polarization spectrum in Galactic molecular clouds has been observed to drop with increasing wavelength between 60 -- 350 \micron. This spectrum requires a model in which the emission arises from dust grains at multiple temperatures along the line of sight and in which the polarizing efficiency of these grains is correlated with their temperature. To test this hypothesis we have estimated the temperature structure in the Orion Molecular Cloud (OMC-1) using far-infrared and submillimeter flux maps. We show that the polarization and temperature data are consistent with our model.
The author(s) of this abstract have provided an email address for comments about the abstract: johnv@wisp.physics.wisc.edu
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Bulletin of the American Astronomical Society, 34, #4
© 2002. The American Astronomical Soceity.