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dc.creatorRao, Ramprasaden_US
dc.creatorPlambeck, Richard L.en_US
dc.creatorWright, M. C. H.en_US
dc.description$^{a}$ M.C.H. Wright, R.L. Plamheck, L.G. Mundy and L.W. Looney Astrophys. J. 455, L185 (1995).en_US
dc.descriptionAuthor Institution: Department of Astronomy, University of Illinois; Radio Astronomy Laboratory, University of Californiaen_US
dc.description.abstractWe mapped the polarization structure of $SiO J=2\to 1$ emission in Orion IRc2 in both the ground state $(v=0)$ and the vibrationally excited state $(v=1)$. The data were obtained using the Berkeley-Illinois-Maryland-Association (BIMA) array at a frequency of 86 GHz. The angular resolution that was achieved was 0.4''. Both the ground state and the vibrationally exited state are associated with maser emission from a disk around a young stellar object (YSO) in $IRc2^{a}$. The $v=1$ emission has 3\% linear polarization which rotates across the spectral line. The fractional linear polarization and the position angle of the plane of polarization vary with time. The v=0 polarized emission seems to arise from a highly compact source but the data show that the polarization angle is constant across the spectrum. In addition, there is no time variability. The data are consistent with a rotating, expanding disk between 40 and 80 AU from a young stellar object (YSO) associated with a radio source (I). The magnetic field is entrained in the disk's motion. At larger radii from source I, the $SiO J=2\to 1 v=0$ traces a flared disk structure on a scale of 1000 AU. The magnetic field on these scales is not strongly influenced by the star formation, or the outflow which is centered on source I. This work was partially funded by NSF grants AST 96-13998, AST96-13999 and by the University of Illinois and the University of California.en_US
dc.format.extent147349 bytes
dc.publisherOhio State Universityen_US

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