Temperature Fluctuations in Photoionized Nebulae in Case of Oxygen and Nitrogen Abundances

DOI: 10.4236/am.2015.62041   PDF   HTML   XML   2,379 Downloads   2,753 Views  


We present the dependence of electron temperature fluctuations of O++ and H+ by the chemical abundances of oxygen and nitrogen. Models assume that hydrogen density is uniform in one case and non uniform in the second case, which vary with the distance from the central star. The abundances of oxygen and nitrogen change by scale factor 5 and 1/5. Our analysis suggests that temperature fluctuations are consistent with photoionization. Using the cloudy photoionization code, we found a reasonable close agreement of the computed value with the one that was done before this work. Our simulation also shows that how change of abundances affects temperature fluctuations and its value is less than 0.01.

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Goshu, S. and Smits, D. (2015) Temperature Fluctuations in Photoionized Nebulae in Case of Oxygen and Nitrogen Abundances. Applied Mathematics, 6, 440-446. doi: 10.4236/am.2015.62041.

Conflicts of Interest

The authors declare no conflicts of interest.


[1] Knigdon, J. and Ferland, G. (1998) Temperature Fluctuations in Photoionized Nebulae. II. The Effect of Inhomogeneous Abundances. The Astrophysical Journal, 506, 323-328.
[2] Peimbert, M. and Torres-Poembert, S. (1971) Planetary Nebulae III. Chemical Abundances. The Astrophysical Journal, 168, 413-421.
[3] Gruenwald, R. and Viegas, S.M. (1995) Temperature Fluctuations in Planetary Nebulae. A & A, 303, 535.
[4] Gonzalez-Delgado, R.M., et al. (1994) Temperature Fluctuations in H II Region. ApJ, 287, 116.
[5] Esteban, RevMexAA(Sc) (2002) Temperature Fluctuations in H Regions.
[6] Ferland, G.J. (2011) Hazy: Introduction to Cloudy c10.00.
[7] Knigdon, J. and Ferland, G. (1995) Temperature Fluctuations in Photoionized Nebulae I. The Astrophysical Journal, 450, 691-704.
[8] Giammanco, C. and Beckman, J.E. (2005) Temperature Fluctuations in H Regions: Ionization by Cosmic Rays as a Key Mechanism. A & A, 437, L11-L14.
[9] Smith, D. (2011) Model of Hydrogen Deficient Nebulae. Astrophysics Journal.
[10] Grevesse, N.A.E. (1989) Solar System Abundances of the Elements. In: AIP conf. proc.183. Cosmic Abundances od Matter.
[11] Torres-Peimbert A & A, 223-540, 1990.
[12] Pequignot.D, J.F.M.M..M.P., W.J. (2002) Henney Ionized Gaseous Nebulae. In: Editors, Eds., Conference Series of the Revisita Mexican de Astrnomiya Y Astrofisica, in Press.
[13] Bresolin, F., Garnett, D.R. and Kennicutt Jr., R.C. (2004) Abundances of Metal-Rich H II Regions in M51. The Astrophysical Journal, 615, 228-241.
[14] Torres-Peimbert, S. and Peimbert, M. (2002) Temperature Variations and Abundances Determinations in Planetary Nebulae. Instituto de Astronom’ia, Universidad Nacional Auto’noma de Me’xico.

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