Physics
Scientific paper
Dec 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7231e&link_type=abstract
HST Proposal ID #7231
Physics
Hst Proposal Id #7231 Young Stars And Circumstellar Material
Scientific paper
Images of H_2, FeII, and Paschen_alpha will be made to characterize processes associated with star formation in Orion. For example, both dissociative and non-dissociative shock models of maser emission have been proposed to explain the existence of the water masers associated with supersonic outflows near young stars. The beaming of maser emission implies there are probably many more masing clumps than we see as masers. We propose to look for these clumps and to determine some of their characteristics. With densities 10^7/cm3 and sizes 3x10^14cm {0.04" at Orion}, non-dissociatively shocked clumps should produce significant H_2 2.12 um line emission, while dissociative shocks should produce detectable FeII 1.64 um emission. The proposed observations will distinguish the two mechanisms, characterize the outflows, provide insights into the process of masing, and diagnose the distribution of ionized and molecular gas excited by nearby young stars. Polarized patterns of extended continuum emission {scattering} can differentiate between foreground, embedded, and background sources, can identify self-luminous sources, can trace magnetic fields, and can probe grain properties. For these purposes, and to clarify the relationship of masing clumps to nearby young stars, we propose polarimetric imaging of some of the same region covered by our spectroscopic imaging program.
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