Spectroscopy and Imagery of the Orion Nebula

Details Spectroscopy and Imagery of the Orion Nebula Spectroscopy and Imagery of the Orion Nebula

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.6056r&link_type=abstract

HST Proposal ID #6056

Physics

Hst Proposal Id #6056 Interstellar Medium

Scientific paper

Recent work has shown that nebular abundances can be in error by as much as a factor of five, possibly due to unexplained temperature fluctuations. We propose a broad program of observations of the benchmark Orion Nebula, with the common theme of understanding the origin of physical conditions on the microscopic scale within this well-observed nebula. We will determine abundances of refractory elements as a function of ionization stage (nebular position). This will allow us to determine the extent of grain destruction and the effects on the thermal balance of the gas. Absorption line studies will permit a more realistic representation of the geometry/density distribution needed for our detailed models. Depending on the actual location of the absorbing matter, abundance assessments may be possible to compare with those deduced from the emission lines. We plan to investigate physical conditions within wind-induced morphology, recently identified, to determine the effects of mechanical heating. The unique resolution of HST will be used to examine Orion on a fine scale to investigate if unresolved (from the ground) ``hot spots'' are present. High excitation lines in the UV (eg. OIII]1663, NII]2142, [FeIV]2836 Angstrom) will permit the measurement of T_e fluctuations for ions never before possible, leading to information on how these depend on the level of ionization or excitation of the gas. All of these goals have as a common underpinning -- understanding the conditions within the nebula and the

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