Axi-symmetrical Planetary Nebular Modeling

Details Axi-symmetrical Planetary Nebular Modeling Axi-symmetrical Planetary Nebular Modeling

Nov 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000ign..confe..29h&link_type=abstract

Ionized Gaseous Nebulae. Mexico City November 21- 24, 2000, meeting abstract

Physics

Scientific paper

When we look for strategically important, often weak, lines, we use a slit spectrograph or an echelle slit entrance and take a narrow pencil through the image. We must, therefore, use the model to predict the emission from this pencil and compare it with the relevant observations. The model program should accommodate this circumstance as long as observers precisely describe the regions they have selected. Thus, we employ a modeling method which involves not just for the calculation of improved models putting in all the best available physics but also development of procedures for predicting the emission from cross-sections taken thru the nebular image. We often see that the planetary nebulae are not spherically symmetrical shells but nebulae with bilateral symmetry. To handle this situation, we developed an axisymmetric photoionization model code which have been applied to determine the abundances of a number of bright planetary nebulae secured with the Lick Hamilton Echelle Spectrograph. We discuss the axi-symmetrical modeling method.

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