Author(s)

Belay S. Goshu^1,2, Derck P. Smits²

¹Dire-Dawa University, Dire-Dawa, Ethiopia.
²Department of Mathematics, Astronomy and Computing Science, UNISA, Pretoria, South Africa.

In current photoionization models, determination of the ionization structure of the nebulae is a crucial part of the calculations for non-uniform hydrogen density. We have been tried to compute temperature fluctuations of electron and electron density by changing hydrogen density by scale factor of 10 at high temperature of blackbody. We have studied the ionization structure of hydrogen and helium by means of cloudy C13.01 codes. We find a reasonable close agreement of the computed value. Moreover, the ionization structure of oxygen at ionization stages of, O I - O IV, in gaseous nebulae are studied by changing non uniform hydrogen density with power law. Our simulation also shows that how the change of this density affect temperature fluctuations, electron density and ionization structures of oxygen, helium and hydrogen with and without grains. The result also shows the impact of the forbidden lines of [O III] and [O II] to cool down the temperature of electron.

H II Regions, Planetary Nebulae, UV, Abundances, Interstellar Medium (ISM)

Goshu, B. and Smits, D. (2015) Model of Hydrogen Deficient Nebulae in H II Regions at High Temperature. Journal of Materials Science and Chemical Engineering, 3, 21-29. doi: 10.4236/msce.2015.38004.