The effect of temperature fluctuations on the determination of the carbon abundance of planetary nebulae.
By combining the C III λλ1906+1909 with the C II λ4267 line intensities it is possible to determine T(C++); this temperature is, in general, considerably smaller than T(O++), the temperature derived from the O III λ4363 to λ5007 intensity ratio. The authors study possible causes for this difference. They show that in the presence of spatial
Peimbert, M. et al.
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1995