Fine Scale Temperature Fluctuations in Gaseous Nebulae

Details Fine Scale Temperature Fluctuations in Gaseous Nebulae Fine Scale Temperature Fluctuations in Gaseous Nebulae

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001hst..prop.9141o&link_type=abstract

HST Proposal ID #9141

Computer Science

Hst Proposal Id #9141 Ism And Circumstellar Matter

Scientific paper

In spite of superb theoretical models for photoionized Galactic and Planetary Nebulae there is a basic problem, known as the t^2 problem, which prevents the accurate determination of relative abundances of the elements. Nebulae are in practice more inhomogeneous in electron temperature than theoretically expected. The purpose of this proposal is to determine just how inhomogeneous the two closest bright exemplars of their class are and what is the source of those inhomogeneities. This will be done by imaging the Orion and Eskimo nebulae in filter sets that will allow determination of O III 5007 and 4363 Angstrom flux ratios, which is a well calibrated electron temperature determinant. We'll use the detailed method of WFPC2 filter calibration developed by the PI, which is necessary since most of the emission line filters do not adequately isolate the emission lines. We'll then compare the zones of high and low electron temperature with the known features in the nebulae, in order to determine if they arise from the best candidates {shock heating and/or shadow cooling}, or an unanticipated process. From these results we expect to be able to estimate the uncertainties in the abundances derived for more distant objects and to suggest corrections for reducing those uncertanties.

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